11institutetext: 1 Max Planck Institute for Extraterrestrial Physics,
Giessenbachstr. 1, D-85748 Garching, Germany
2 Universitäts-Sternwarte München, Fakultät für Physik, Ludwig-Maximilians-
Universität München, Scheinerstrasse 1, 81679 München, Germany
3 INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via
Piero Gobetti 93/3, I-40129 Bologna, Italy
4 Landessternwarte, Zentrum für Astronomie der Universität Heidelberg,
Königstuhl 12, 69117 Heidelberg, Germany
5 Infrared Processing and Analysis Center, California Institute of Technology,
Pasadena, CA 91125, USA
6 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak
Grove Drive, Pasadena, CA, 91109, USA
7 Department of Astronomy, University of Geneva, ch. dÉcogia 16, CH-1290
Versoix, Switzerland
8 Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth
PO1 3FX, UK
9 Dipartimento di Fisica e Astronomia, Universitá di Bologna, Via Gobetti
93/2, I-40129 Bologna, Italy
10 INFN-Sezione di Bologna, Viale Berti Pichat 6/2, I-40127 Bologna, Italy
11 INAF-Osservatorio Astrofisico di Torino, Via Osservatorio 20, I-10025 Pino
Torinese (TO), Italy
12 Dipartimento di Fisica, Universitá degli studi di Genova, and INFN-Sezione
di Genova, via Dodecaneso 33, I-16146, Genova, Italy
13 INFN-Sezione di Roma Tre, Via della Vasca Navale 84, I-00146, Roma, Italy
14 INAF-Osservatorio Astronomico di Capodimonte, Via Moiariello 16, I-80131
Napoli, Italy
15 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP,
Rua das Estrelas, PT4150-762 Porto, Portugal
16 Dipartimento di Fisica, Universitá degli Studi di Torino, Via P. Giuria 1,
I-10125 Torino, Italy
17 INFN-Sezione di Torino, Via P. Giuria 1, I-10125 Torino, Italy
18 INAF-IASF Milano, Via Alfonso Corti 12, I-20133 Milano, Italy
19 Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of
Science and Technology, Campus UAB, 08193 Bellaterra (Barcelona), Spain
20 Port d’Informació Científica, Campus UAB, C. Albareda s/n, 08193 Bellaterra
(Barcelona), Spain
21 INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00078 Monteporzio
Catone, Italy
22 INFN section of Naples, Via Cinthia 6, I-80126, Napoli, Italy
23 Department of Physics ”E. Pancini”, University Federico II, Via Cinthia 6,
I-80126, Napoli, Italy
24 Institut national de physique nucléaire et de physique des particules, 3
rue Michel-Ange, 75794 Paris Cédex 16, France
25 Institute for Astronomy, University of Edinburgh, Royal Observatory,
Blackford Hill, Edinburgh EH9 3HJ, UK
26 Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy,
University of Manchester, Oxford Road, Manchester M13 9PL, UK
27 ESAC/ESA, Camino Bajo del Castillo, s/n., Urb. Villafranca del Castillo,
28692 Villanueva de la Cañada, Madrid, Spain
28 European Space Agency/ESRIN, Largo Galileo Galilei 1, 00044 Frascati, Roma,
Italy
29 Univ Lyon, Univ Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822,
F-69622, Villeurbanne, France
30 Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique
Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix,
Switzerland
31 Mullard Space Science Laboratory, University College London, Holmbury St
Mary, Dorking, Surrey RH5 6NT, UK
32 Departamento de Física, Faculdade de Ciências, Universidade de Lisboa,
Edifício C8, Campo Grande, PT1749-016 Lisboa, Portugal
33 Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências,
Universidade de Lisboa, Campo Grande, PT-1749-016 Lisboa, Portugal
34 Université Paris-Saclay, CNRS, Institut d’astrophysique spatiale, 91405,
Orsay, France
35 Department of Physics, Oxford University, Keble Road, Oxford OX1 3RH, UK
36 INFN-Padova, Via Marzolo 8, I-35131 Padova, Italy
37 AIM, CEA, CNRS, Université Paris-Saclay, Université de Paris, F-91191 Gif-
sur-Yvette, France
38 INAF-Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, I-34143
Trieste, Italy
39 Aix-Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France
40 Istituto Nazionale di Astrofisica (INAF) - Osservatorio di Astrofisica e
Scienza dello Spazio (OAS), Via Gobetti 93/3, I-40127 Bologna, Italy
41 Istituto Nazionale di Fisica Nucleare, Sezione di Bologna, Via Irnerio 46,
I-40126 Bologna, Italy
42 INAF-Osservatorio Astronomico di Padova, Via dell’Osservatorio 5, I-35122
Padova, Italy
43 Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029
Blindern, N-0315 Oslo, Norway
44 Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The
Netherlands
45 von Hoerner & Sulger GmbH, SchloßPlatz 8, D-68723 Schwetzingen, Germany
46 Technical University of Denmark, Elektrovej 327, 2800 Kgs. Lyngby, Denmark
47 Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg,
Germany
48 Université de Genève, Département de Physique Théorique and Centre for
Astroparticle Physics, 24 quai Ernest-Ansermet, CH-1211 Genève 4, Switzerland
49 Department of Physics and Helsinki Institute of Physics, Gustaf Hällströmin
katu 2, 00014 University of Helsinki, Finland
50 European Space Agency/ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, The
Netherlands
51 NOVA optical infrared instrumentation group at ASTRON, Oude Hoogeveensedijk
4, 7991PD, Dwingeloo, The Netherlands
52 Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71,
53121 Bonn, Germany
53 Dipartimento di Fisica e Astronomia ”Augusto Righi” - Alma Mater Studiorum
Università di Bologna, via Piero Gobetti 93/2, I-40129 Bologna, Italy
54 Department of Physics, Institute for Computational Cosmology, Durham
University, South Road, DH1 3LE, UK
55 Institut d’Astrophysique de Paris, UMR 7095, CNRS, and Sorbonne Université,
98 bis boulevard Arago, 75014 Paris, France
56 University of Applied Sciences and Arts of Northwestern Switzerland, School
of Engineering, 5210 Windisch, Switzerland
57 Department of Physics and Astronomy, University of Aarhus, Ny Munkegade
120, DK-8000 Aarhus C, Denmark
58 Centre for Astrophysics, University of Waterloo, Waterloo, Ontario N2L 3G1,
Canada
59 Department of Physics and Astronomy, University of Waterloo, Waterloo,
Ontario N2L 3G1, Canada
60 Perimeter Institute for Theoretical Physics, Waterloo, Ontario N2L 2Y5,
Canada
61 Université Paris-Saclay, Université Paris Cité, CEA, CNRS, Astrophysique,
Instrumentation et Modélisation Paris-Saclay, 91191 Gif-sur-Yvette, France
62 Centre National d’Etudes Spatiales, Toulouse, France
63 Institute of Space Science, Bucharest, Ro-077125, Romania
64 Dipartimento di Fisica e Astronomia ”G.Galilei”, Universitá di Padova, Via
Marzolo 8, I-35131 Padova, Italy
65 Departamento de Física, FCFM, Universidad de Chile, Blanco Encalada 2008,
Santiago, Chile
66 IFPU, Institute for Fundamental Physics of the Universe, via Beirut 2,
34151 Trieste, Italy
67 Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas
(CIEMAT), Avenida Complutense 40, 28040 Madrid, Spain
68 Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências,
Universidade de Lisboa, Tapada da Ajuda, PT-1349-018 Lisboa, Portugal
69 Universidad Politécnica de Cartagena, Departamento de Electrónica y
Tecnología de Computadoras, 30202 Cartagena, Spain
70 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700
AV Groningen, The Netherlands
71 INAF-Osservatorio Astronomico di Brera, Via Brera 28, I-20122 Milano, Italy
72 Dipartimento di Fisica ”Aldo Pontremoli”, Universitá degli Studi di Milano,
Via Celoria 16, I-20133 Milano, Italy
73 INFN-Sezione di Milano, Via Celoria 16, I-20133 Milano, Italy
74 Dipartimento di Fisica e Astronomia ”Augusto Righi” - Alma Mater Studiorum
Universitá di Bologna, Viale Berti Pichat 6/2, I-40127 Bologna, Italy
75 INFN, Sezione di Trieste, Via Valerio 2, I-34127 Trieste TS, Italy
76 SISSA, International School for Advanced Studies, Via Bonomea 265, I-34136
Trieste TS, Italy
77 Instituto de Astrofísica de Canarias (IAC); Departamento de Astrofísica,
Universidad de La Laguna (ULL), E-38200, La Laguna, Tenerife, Spain
78 Instituto de Astrofísica de Canarias, Calle Vía Láctea s/n, E-38204, San
Cristóbal de La Laguna, Tenerife, Spain
79 INFN-Bologna, Via Irnerio 46, I-40126 Bologna, Italy
80 Dipartimento di Fisica e Scienze della Terra, Universitá degli Studi di
Ferrara, Via Giuseppe Saragat 1, I-44122 Ferrara, Italy
81 INAF, Istituto di Radioastronomia, Via Piero Gobetti 101, I-40129 Bologna,
Italy
82 Institut d’Astrophysique de Paris, 98bis Boulevard Arago, F-75014, Paris,
France
83 Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire
Lagrange, Bd de l’Observatoire, CS 34229, 06304 Nice cedex 4, France
84 Institute for Theoretical Particle Physics and Cosmology (TTK), RWTH Aachen
University, D-52056 Aachen, Germany
85 Department of Physics & Astronomy, University of California Irvine, Irvine
CA 92697, USA
86 University of Lyon, UCB Lyon 1, CNRS/IN2P3, IUF, IP2I Lyon, France
87 INFN-Sezione di Genova, Via Dodecaneso 33, I-16146, Genova, Italy
88 INAF-Istituto di Astrofisica e Planetologia Spaziali, via del Fosso del
Cavaliere, 100, I-00100 Roma, Italy
89 School of Physics, HH Wills Physics Laboratory, University of Bristol,
Tyndall Avenue, Bristol, BS8 1TL, UK
90 Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris,
France
91 Departamento de Física Teórica, Facultad de Ciencias, Universidad Autónoma
de Madrid, 28049 Cantoblanco, Madrid, Spain
92 Instituto de Física Teórica UAM-CSIC, Campus de Cantoblanco, E-28049
Madrid, Spain
93 Department of Physics, P.O. Box 64, 00014 University of Helsinki, Finland
94 Ruhr University Bochum, Faculty of Physics and Astronomy, Astronomical
Institute (AIRUB), German Centre for Cosmological Lensing (GCCL), 44780
Bochum, Germany
95 Department of Physics, Lancaster University, Lancaster, LA1 4YB, UK
96 Aix-Marseille Univ, CNRS, CNES, LAM, Marseille, France
97 Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771 and SSAI,
Lanham, MD 20770, USA
98 Astrophysics Group, Blackett Laboratory, Imperial College London, London
SW7 2AZ, UK
99 Department of Physics and Astronomy, University College London, Gower
Street, London WC1E 6BT, UK
100 Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, 53, Avenue des
Martyrs, 38000, Grenoble, France
101 Centre de Calcul de l’IN2P3, 21 avenue Pierre de Coubertin F-69627
Villeurbanne Cedex, France
102 Dipartimento di Fisica, Sapienza Università di Roma, Piazzale Aldo Moro 2,
I-00185 Roma, Italy
103 Department of Mathematics and Physics E. De Giorgi, University of Salento,
Via per Arnesano, CP-I93, I-73100, Lecce, Italy
104 INAF-Sezione di Lecce, c/o Dipartimento Matematica e Fisica, Via per
Arnesano, I-73100, Lecce, Italy
105 INFN, Sezione di Lecce, Via per Arnesano, CP-193, I-73100, Lecce, Italy
106 Institute for Computational Science, University of Zurich,
Winterthurerstrasse 190, 8057 Zurich, Switzerland
107 Higgs Centre for Theoretical Physics, School of Physics and Astronomy, The
University of Edinburgh, Edinburgh EH9 3FD, UK
108 Université St Joseph; Faculty of Sciences, Beirut, Lebanon
109 Institut de Recherche en Astrophysique et Planétologie (IRAP), Université
de Toulouse, CNRS, UPS, CNES, 14 Av. Edouard Belin, F-31400 Toulouse, France
110 Department of Astrophysical Sciences, Peyton Hall, Princeton University,
Princeton, NJ 08544, USA
111 Department of Physics, P.O.Box 35 (YFL), 40014 University of Jyväskylä,
Finland
112 Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of
Helsinki, Helsinki, Finland
113 Department of Mathematics and Physics, Roma Tre University, Via della
Vasca Navale 84, I-00146 Rome, Italy

#  Euclid preparation: XX. The Complete Calibration of the Color–Redshift
Relation survey: LBT observations and data release ††thanks: The LBT is an
international collaboration among institutions in the United States, Italy,
and Germany. The LBT Corporation partners are: LBT Beteiligungsgesellschaft,
Germany, representing the Max-Planck Society, the Astrophysical Institute
Potsdam, and Heidelberg University; The University of Arizona on behalf of the
Arizona university system; Istituto Nazionale di Astrofisica, Italy; The Ohio
State University, and The Research Corporation, on behalf of The University of
Notre Dame, University of Minnesota, and University of Virginia.

Euclid Collaboration: R. Saglia0000-0003-0378-70321,2<EMAIL_ADDRESS>S. De
Nicola1 M. Fabricius1 V. Guglielmo3 J. Snigula1 R. Zöller1,2 R. Bender1,2 J.
Heidt4 D. Masters5 D. Stern0000-0003-2686-92416 S. Paltani0000-0002-8108-91797
A. Amara8 N. Auricchio3 M. Baldi0000-0003-4145-19439,3,10 C. Bodendorf1 D.
Bonino11 E. Branchini12,13 M. Brescia0000-0001-9506-568014 J.
Brinchmann0000-0003-4359-879715 S. Camera0000-0003-3399-357416,17,11 V.
Capobianco0000-0002-3309-769211 C. Carbone18 J.
Carretero0000-0002-3130-020419,20 M. Castellano0000-0001-9875-826321 S.
Cavuoti0000-0002-3787-419614,22,23 R. Cledassou0000-0002-8313-223024 G.
Congedo0000-0003-2508-004625 C.J. Conselice26 L. Conversi27,28 Y.
Copin0000-0002-5317-751829 L. Corcione0000-0002-6497-588111 F.
Courbin0000-0003-0758-651030 M. Cropper0000-0003-4571-946831 A. Da Silva32,33
H. Degaudenzi0000-0002-5887-67997 M. Douspis34 F. Dubath7 C.A.J. Duncan35 X.
Dupac27 S. Dusini0000-0002-1128-066436 S. Farrens0000-0002-9594-938737 M.
Frailis0000-0002-7400-213538 E. Franceschi0000-0002-0585-65913 S.
Galeotta0000-0002-3748-511538 B. Garilli0000-0001-7455-875018 W. Gillard39 B.
Gillis0000-0002-4478-127025 C. Giocoli0000-0002-9590-796140,41 A.
Grazian0000-0002-5688-066342 F. Grupp1,2 S.V.H. Haugan0000-0001-9648-726043 H.
Hoekstra0000-0002-0641-323144 W. Holmes6 F. Hormuth45 A. Hornstrup46 K.
Jahnke0000-0003-3804-213747 M. Kümmel2 S. Kermiche0000-0002-0302-573539 A.
Kiessling6 M. Kunz0000-0002-3052-739448 H. Kurki-Suonio49 R. Laureijs50 S.
Ligori0000-0003-4172-460611 P. B. Lilje0000-0003-4324-779443 I. Lloro51 E.
Maiorano0000-0003-2593-43553 O. Marggraf0000-0001-7242-385252 K.
Markovic0000-0001-6764-073X6 F. Marulli0000-0002-8850-030353,3,10 R.
Massey0000-0002-6085-378054 H.J. McCracken0000-0002-9489-776555 M. Melchior56
G. Meylan30 M. Moresco0000-0002-7616-713653,3 L.
Moscardini0000-0002-3473-671653,3,10 E. Munari0000-0002-1751-594638 S.M.
Niemi50 C. Padilla0000-0001-7951-016619 F. Pasian38 K. Pedersen57 W.J.
Percival58,59,60 V. Pettorino61 S. Pires37 M. Poncet62 L. Popa63 L.
Pozzetti0000-0001-7085-04123 F. Raison1 A. Renzi0000-0001-9856-197064,36 J.
Rhodes6 G. Riccio14 E. Romelli0000-0003-3069-922238 E. Rossetti53 D. Sapone65
B. Sartoris66,38 P. Schneider52 A. Secroun0000-0003-0505-371039 G.
Seidel0000-0003-2907-353X47 C. Sirignano0000-0002-0995-714664,36 G.
Sirri0000-0003-2626-285310 L. Stanco36 P. Tallada-Crespí67,20 D.
Tavagnacco0000-0001-7475-989438 A.N. Taylor25 I. Tereno32,68 R. Toledo-
Moreo0000-0002-2997-485969 F. Torradeflot67,20 I.
Tutusaus0000-0002-3199-039948 E.A. Valentijn70 L. Valenziano3,10 T.
Vassallo0000-0001-6512-635838 Y. Wang0000-0002-4749-29845 A.
Zacchei0000-0003-0396-119238 G. Zamorani0000-0002-2318-301X3 J. Zoubian39 S.
Andreon0000-0002-2041-878471 S. Bardelli0000-0002-8900-02983 J. Graciá-Carpio1
D. Maino72,18,73 N. Mauri74,10 A. Tramacere7 E. Zucca0000-0002-5845-81323 A.
Alvarez Ayllon0000-0002-1353-79297 H. Aussel0000-0002-1371-570537 C.
Baccigalupi0000-0002-8211-163066,38,75,76 A. Balaguera-Antolínez77,78 M.
Ballardini53,3,79 A. Biviano0000-0002-0857-073238,66 M.
Bolzonella0000-0003-3278-460740 E. Bozzo0000-0002-8201-15257 C.
Burigana0000-0002-3005-579680,81,79 R. Cabanac0000-0001-6679-260082 A.
Cappi83,3 C.S. Carvalho68 S. Casas0000-0002-4751-513884 G. Castignani53,3 A.
Cooray85 J. Coupon7 H.M. Courtois0000-0003-0509-177686 S. Davini87 G. Desprez7
H. Dole0000-0002-9767-383934 J.A. Escartin1 S. Escoffier0000-0002-2847-749839
M. Farina88 S. Fotopoulou89 K. Ganga0000-0001-8159-820890 J. Garcia-
Bellido0000-0002-9370-836091,92 K. George0000-0002-1734-84552 F.
Giacomini0000-0002-3129-281410 G. Gozaliasl0000-0002-0236-919X93 H.
Hildebrandt0000-0002-9814-333894 I. Hook0000-0002-2960-978X95 O. Ilbert96,6,5
V. Kansal37 A. Kashlinsky97 E. Keihanen93 C.C. Kirkpatrick49 A.
Loureiro0000-0002-4371-087698,25,99 J. Macías-Pérez0000-0002-5385-2763100 M.
Magliocchetti0000-0001-9158-483888 G. Mainetti101 R. Maoli102,21 M.
Martinelli0000-0002-6943-773221 N. Martinet0000-0003-2786-779096 R. B.
Metcalf0000-0003-3167-257453,3 G. Morgante3 S. Nadathur0000-0001-9070-31028
A.A. Nucita103,104,105 L. Patrizii10 V. Popa63 C. Porciani52 D.
Potter0000-0002-0757-5195106 A. Pourtsidou0000-0001-9110-5550107,25 P.
Reimberg82 A.G. Sánchez0000-0003-1198-831X1 Z. Sakr0000-0002-4823-3757108,109
M. Schirmer0000-0003-2568-999447 E. Sefusatti0000-0003-0473-156738,66,75 M.
Sereno0000-0003-0302-03253,10 J. Stadel0000-0001-7565-8622106 R. Teyssier110
C. Valieri10 J. Valiviita0000-0001-6225-3693111,112 A.
Veropalumbo0000-0003-2387-1194113,13 M. Viel0000-0002-2642-570766,38,75,76

(Received xxx; accepted yyy)

The Complete Calibration of the Color–Redshift Relation survey (C3R2) is a
spectroscopic program designed to empirically calibrate the galaxy
color–redshift relation to the Euclid depth ($I_{\scriptscriptstyle{\rm
E}}=24.5$), a key ingredient for the success of Stage IV dark energy projects
based on weak lensing cosmology. A spectroscopic calibration sample that is as
representative as possible of the galaxies in the Euclid weak lensing sample
is being collected, selecting galaxies from a self-organizing map (SOM)
representation of the galaxy color space. Here, we present the results of a
near-infrared $H$\- and $K$-band spectroscopic campaign carried out using the
LUCI instruments at the LBT. For a total of 251 galaxies, we present new
highly reliable redshifts in the $1.3\leq z\leq 1.7$ and $2\leq z\leq 2.7$
ranges. The newly-determined redshifts populate 49 SOM cells that previously
contained no spectroscopic measurements and almost twice the occupation
numbers of an additional 153 SOM cells. A final optical ground-based
observational effort is needed to calibrate the missing cells, in particular
in the redshift range $1.7\leq z\leq 2.7$, which t lack spectroscopic
calibration. In the end, Euclid itself will deliver telluric-free near-IR
spectra that can complete the calibration.

###### Key Words.:

astronomical databases: catalogs - astronomical databases: surveys -
cosmology: observations - galaxies: distances and redshifts

##  1 Introduction

The Euclid satellite (Laureijs et al., 2011) is scheduled for launch in 2023;
it will observe galaxies to $z>2$ over $15\,000\,\rm deg^{2}$ using two
instruments: VIS, an optical imager that will reach an AB magnitude depth of
24.5 (for extended sources at $10-\sigma$, see also Euclid Collaboration:
Scaramella et al., 2021) with a single broad $I_{\scriptscriptstyle{\rm E}}$
filter, and NISP, a combined near-infrared imager (in
$Y_{\scriptscriptstyle{\rm E}}$, $J_{\scriptscriptstyle{\rm E}}$, and
$H_{\scriptscriptstyle{\rm E}}$, see Euclid Collaboration: Schirmer et al.,
2022) and slitless spectrograph. The optical imager will determine galaxy
shape distortions with unprecedented accuracy. When combined with a precise
determination of the true ensemble redshift distribution, this allows the weak
lensing effects caused by the distribution of matter along the line of sight
to be measured and the cosmological parameters to be constrained (Euclid
Collaboration: Blanchard et al., 2020).

The estimated number of weak lensing source galaxies that will be imaged from
Euclid makes their systematic spectroscopic follow-up unfeasible; this mission
is thus critically dependent upon the determination of accurate photometric
redshifts ($z_{\rm phot}$). Currently, the precision of photometric redshifts
based on multi-band optical surveys is to the order of
$\sigma_{z}/(1+z)=0.03-0.06,$ and the fraction of catastrophic outliers, which
are defined as objects whose $z_{\rm phot}$ differs from their spectroscopic
redshift ($z_{\rm spec}$) by more than $0.15(1+z),$ is of the order of a few
tens of percent (Ma et al., 2006; Hildebrandt et al., 2010). We expect that
the combination of ground-based optical and Euclid near-infrared photometry
will deliver the slightly improved requirements of the mission:
$\sigma_{z}/(1+z)\leq 0.05,$ and a fraction of catastrophic outliers less than
10% (see Laureijs et al. 2011 and Euclid Collaboration: Desprez et al. 2020).

While small changes in $z_{\rm phot}$ precision per source have a relatively
small impact on cosmological parameter estimates, small systematic errors in
$z_{\rm phot}$ can dominate all other uncertainties for these experiments. The
aim of the C3R2 project (Masters et al., 2015, 2017, 2019; Euclid
Collaboration: Guglielmo et al., 2020; Euclid Collaboration: Stanford et al.,
2021) is to calibrate photometric redshifts by measuring accurate
spectroscopic redshifts of selected objects sampling a self-organizing map
(SOM), a representation of the galaxy color space. The SOM projects the high-
dimensional galaxy color space onto a 2D plane. Each galaxy is assigned to a
cell in this plane with given coordinates $(X,Y)$. If this plane is sampled
with enough cells, the distribution of photometric redshifts of all galaxies
belonging to a cell is narrow and there is a well-defined correspondence
between the position occupied by a galaxy in the multi-color space and its
redshift. We can define $z_{\rm phot,SOM}$ as the average of the photometric
redshifts of all galaxies belonging to the cell. By measuring spectroscopic
redshifts of galaxies in each cell it is possible to calibrate the mean of the
photometric redshift distribution in an efficient and homogeneous way across
the galaxy color space. Regions in color space particularly difficult to
calibrate because of broad or bimodal photometric redshift distributions can
be identified by comparing the measured spectroscopic redshifts with $z_{\rm
phot,SOM}$ and looking for deviations larger than $0.15(1+z)$. The minimum
calibration requirement is to populate each SOM cell with at least one
spectroscopic redshift; problematic cells might require (much) more than this.
Ultimately, galaxies belonging to uncalibrated cells may be dropped from the
Euclid weak lensing sample; for a detailed discussion see Masters et al.
(2015).

In this work we continue this effort by presenting the redshift measurements
of $z>1$ galaxies collected at the Large Binocular Telescope (LBT) in the
COSMOS (Capak et al., 2007; Scoville et al., 2007; Lilly et al., 2007) and
VVDS (McCracken et al., 2003; Le Fèvre et al., 2004; Jarvis et al., 2013)
fields, using the near-infrared LUCI spectrographs. Further data releases of
optical spectra acquired at the VLT and the GRANTECAN telescopes are in
preparation. The Euclid science working groups are actively discussing how the
final ground-based dataset will be merged with the spectroscopy information
delivered by the Euclid mission itself to perform the optimal calibration of
the photometric redshifts.

The paper is organized as follows: in Sect. 2 we describe the strategy, target
selection, and mask preparation; in Sect. 3 we describe the observations and
data reduction; in Sect. 4 we discuss the redshift determination and the
attribution of a flagging scheme consistent over the whole C3R2 survey; in
Sect. 5 we present the results of the redshift assignments, and we investigate
the bias of the photometric redshifts using in C3R2 and the origin of
catastrophic SOM redshifts, and we discuss our success rate and SOM cell
coverage; finally, we present our conclusions in Sect. 6.

Figure 1: COSMOS_M25H mask designed with the lms tool. The white square shows
the LUCI field of view $(4\times 4\,{\rm arcmin}^{2})$, the long-dashed
vertical lines bracket the optimal field of view for spectroscopy (2.8 arcmin
wide). The green circle at the center of the field allows the mask to be
moved. The cyan circles identify the alignment stars. The yellow rectangles
show the slits; slit number 25 is positioned on an acquisition star to monitor
seeing and transparency during the observations. The square slit number 26,
also positioned on an acquisition star, allows verification of the centering
of the mask after alignment. At the lower end of the mask, a series of six
small holes is present for engineering purposes. Below these, the red
rectangle is the area occupied by the identification number cut into the mask.
Figure 2: COSMOS_M25K mask (see Fig. 1 for a description). Most of the slits
are assigned to different objects.

##  2 Strategy, target selection, and mask preparation

The LBT consists of two 8 m mirrors mounted on a common structure and pointing
at the same position on the sky. The LUCI1 and LUCI2 near-infrared
spectrographs (Seifert et al., 2003) are mounted at the front Bent Gregorian
f/15 focal stations of the LBT, and can be used in combination with masks
(Buschkamp et al., 2010), designed and cut well in advance of the
observations, that allow the simultaneous collection of multiple spectra. The
field must be observed with identical pointings and rotation angles, but
potentially with different masks and instrumental setups on the two sides. The
masks cover a $4\times 4\,{\rm arcmin}^{2}$ field of view, but only for slits
placed in a 2.8 arcmin wide central stripe are optimally focused spectra
delivered. Moreover, the wavelength range covered depends on the distance of a
slit from the middle of a mask. At least three stars are needed to align the
masks. Dedicated holes (typically $4\times 4\,{\rm arcsec}^{2}$ big) were
required until the June 2020 runs. Starting from the July 2020 run, after a
change in requirements from the observatory, only one hole was necessary.

###  2.1 Strategy

Given the characteristics of the LBT and of the LUCI spectrographs described
above, and following the strategy adopted by Euclid Collaboration: Guglielmo
et al. (2020) (hereafter G2020), we collected spectra in the $H$ and $K$
bands. In the $H$ band we can measure spectroscopic redshifts of galaxies
between 1.3 and 1.7 by detecting their H$\alpha$, [N ii], and [S ii] emission
lines, or of galaxies with redshifts between 2 and 2.7 by detecting their
H$\beta$ and [O iii] lines. In the $K$ band we can measure spectroscopic
redshifts of galaxies between 2 and 2.7 by detecting their H$\alpha$, [N ii],
and [S ii] emission lines, or (in principle) of galaxies with photometric
redshifts less than 1.7 by detecting their Paschen (hereafter Pa) lines. We
used the N1.8 camera, which delivers $0.25\times 0.25\,{\rm arcsec}^{2}$ per
pixels, and the G210 gratings, for which 1 arcsec-wide slits give a resolution
of $R=2950$ in the $H$ band and $R=2500$ in the $K$ band. The nominal
wavelength range for a centered slit is 0.202 $\mu$m and 0.328 $\mu$m in the
$H$ and $K$ band, respectively. The central wavelength can be adjusted in the
range 1.55 to 1.75 $\mu$m for the $H$ band, and 2.06 to 2.40 $\mu$m for the
$K$ band. We optimized the central wavelength for each mask separately, based
on the photometric redshifts of the observed galaxies, to maximize the likely
return.

The typical angular size of the galaxies in the C3R2 catalogues is 1–2 arcsec
in diameter. In order to achieve maximum efficiency avoiding separate sky
observations, we opted for an on-slit nodding strategy, which sets the default
slit length to 10 arcsec and forces all slits to be parallel. Taking into
account the minimum allowed distance between slits, and the necessity of
cutting holes for acquisition stars, the maximum number of galaxies targeted
per mask is $\approx 20$. In reality, we never managed to observe more than 18
galaxies per mask. We ranked the list of positions and rotation angles
according to the total number of galaxies observable simultaneously in the $H$
and $K$ bands. We observed the VVDS field in October and the COSMOS field in
the months from December to May. We ended up with a list of 13 pairs of
($H+K$) masks in the VVDS field, and 28 pairs of ($H+K$) masks in the COSMOS
field, for which at least a total ($H+K$) 20 galaxies could be assigned,
minimizing the number of repeated observations. As in G2020, we aimed to
observe each mask for 2 hours, split into 36 exposures of 200 s each,
dithering the mask along the slits by 2 arcsec following an ABBA pattern. The
actual number of exposures collected for each mask varied according to
observational conditions and constraints; see Table 3.

###  2.2 Target selection and mask preparation

The selection of galaxies to be observed started from the catalogues produced
by Masters et al. (2019) and used by G2020, excluding galaxies already
observed with KMOS at the VLT. The catalogues adopt the photometric redshifts
provided by Ilbert et al. (2006) and Laigle et al. (2016). We considered
Priority 1 and Priority 2 galaxies (hereafter primary galaxies), as in G2020,
and mapped the number of galaxies assignable to each mask as a function of the
coordinates of the field centers and rotation angles, taking into
consideration several constraints. At least one suitable guiding star had to
be present in the allowed patrol field and within the appropriate magnitude
range; at least three acquisition stars (preferably selected to have low
proper motions) within the appropriate magnitude range should be present in
the $4\times 4\,{\rm arcmin}^{2}$ field of view; at least three $4\times
4\,{\rm arcsec}^{2}$ holes (or just one from October 2020) were cut for this
purpose. At least one $10\times 1\,{\rm arcsec}^{2}$ slit was assigned to a
star, to be able to reconstruct empirically the dithering pattern and measure
the seeing and the relative transparency during the observations. The galaxies
were placed such that the expected H$\alpha$ line based on their photometric
redshift fell into the wavelength range computed based on the distance to the
central stripe of the field and the optimized central wavelength.

The actual design of the masks was performed with the lms
tool111https://sites.google.com/a/lbto.org/luci/preparing-to-observe/mask-
preparation/lms-install. During this phase, further tweakings of the centers,
position angles, and slit assignments were necessary. Guide stars too near the
border of the patrol field had to be changed, some acquisition stars or some
slits had to be dropped or changed in length (down to 7 arcsec) because of
additional constraints (e.g., one end of the mask has a regular pattern of
small holes that must be avoided). Finally, the space available between the
slits was filled manually with secondary galaxies, when possible. These are
galaxies where the [O iii] lines could possibly appear in the $H$ band, or the
Pa lines in the $K$ band. Once the list of Priority 1 and 2 galaxies assigned
to each mask was ready, the optimal central wavelength was calculated as the
average of the H$\alpha$ wavelengths, redshifted with the respective
photometric redshifts. The gbr files detailing the masks for the cutting
machine were passed to the observatory, where the masks were produced and
inserted into the cryostatic dewar before each observing run.

An example of a pair of $H+K$ masks is given in the Figs. 1 and 2. All the
observed masks are listed in Table 3, where the coordinates of their centers
and of their rotation angles, together with the date of the observations are
given. In the end (see Table 3), on average we extracted 12.3 galaxy spectra
per mask, of which on average 9.6 were primary.

##  3 Observations and data reduction

The scripts controlling the telescope and LUCI operations were prepared using
the LBTO OT software222https://sites.google.com/a/lbto.org/observing-tool-
manual/observing-tool/ot-installation. Except when one of the two LUCI
spectrographs was not available, the paired approach was adopted, allowing
simultaneous observation of the same field in the $H$ and $K$ bands. Monocular
scripts were prepared for the October 2019 run (when only LUCI1 was available)
and for the January 2020 run (when LUCI1 became unavailable during the run).
Monocular scripts were also prepared for the observations of telluric
standards. Calibration scripts to obtain dark, flat, and arc observations were
also prepared in paired mode and performed during the day or at night during
periods of bad weather. The observations started in visitor mode (October
2019), and continued in remote observing mode as the COVID19 emergency made
international traveling impossible. Staff members from the LBT Observatory
operated the instrument from Tucson for all observing runs, with scientists
from the Max Planck Institute for extraterrestrial physics (M. Fabricius, S.
de Nicola, R. Saglia, J. Snigula) and the Landessternwarte (J. Heidt) mainly
supervising, but also directly controlling the procedures from Germany.
Overall, the VVDS field was observed under good meteorological conditions; in
contrast, several nights during which the COSMOS field was observed (in
particular the March 2021 run), suffered from cirrus, high winds, and poor
seeing.

The observation of a field follows four steps. First, an image is taken
without the mask at each telescope, the acquisition stars are identified, and
their positions are measured. Second, the best-fitting field rotations and
translations are determined separately for the two images and applied,
possibly culling the most deviant acquisition stars. Third, a second pair of
images is taken through the mask to verify that acquisition and seeing-
monitoring stars appear in the appropriate holes and slits. If necessary, a
second translation is determined and applied to optimize the centering
orthogonal to the slits. The achieved RMS precision of the alignment was
typically between 0.1 and 0.3 arcsec. Fourth, the spectroscopic observations
start.

After the observation of a field, or before the observation of the next one, a
telluric standard was observed separately for the $H$ and $K$ band, putting
the standard star sequentially in three slits of each mask, selected to cover
the whole probed wavelength range. We observed a total of 88 masks (58 in the
COSMOS field and 30 in the VVDS field), 47 in the $H$ band (30 in the COSMOS
field and 17 in the VVDS field), and 41 in the $K$ band (28 in the COSMOS
field and 13 in the VVDS field). As mentioned above, during the October 2019
run, LUCI2 was unavailable, and during the January 2020 run LUCI1 stopped
working.

The data reduction was performed using the IDL Flame pipeline developed by
Belli et al. (2018). We used the configuration which relies on the science
data for tracing, extraction, and wavelength calibration, exploiting the
brightness of the sky background. The steps follow the sequence described in
Belli et al. (2018). First, the position of the reference star on each frame
is searched for and, if detected, the flux, vertical position, and full width
at half maximum (FWHM) are measured. This allows the determination of the
nodding and dithering offsets of each A and B frame in the ABBA sequences.
However, for many of the $K$-band pointings, the reference star cannot be
detected in single frames and appears visible only after the coaddition is
performed. In these cases, the list of the nominal shifts is used. After
application of the bad pixel and master pixel maps, a master slit flat is
computed and used to identify the slit positions and map their edges. Cutouts
of the slits are produced and, after a rough wavelength calibration,
individual OH emission lines are identified and fitted with a Gaussian. The
relation between pixel position and wavelength is determined as a second-order
polynomial for each slit row. The spatial illumination correction is
determined from the detected OH lines and applied. A model of the sky is
constructed following Kelson (2003) and subtracted. Finally, each sky-
subtracted slit frame is rectified and wavelength calibrated before all the A
and B frames are stacked together and the A-B and B-A results are produced.
Their combination gives the final 2D spectra shown in Figs. 3 and 4. One-
dimensional spectra are extracted after having identified the appropriate
spatial window, either determining the spatial extent of the emission lines or
of the continuum. Examples are shown in Figs. 3 and 4. We note that
wavelengths refer to the vacuum and do not take into account the barycentric
correction, which is applied a posteriori to the measured redshift.

##  4 Redshift determination and flagging

Redshifts are measured on the 1D spectra after having spotted by eye the
signatures of emission lines on the 2D spectra: the presence of a sequence of
a negative (black), a positive (white), and a negative (black) blob (see Figs.
3 and 4). Based on the alignment of the predicted positions of H$\alpha$, [N
ii], [S ii], H$\beta$, [O iii], or Pa lines with the peaks of the observed
emission lines, an estimate of the redshift of the galaxy is derived, together
with the appropriate flag. Following the scheme used in G2020, a ${\rm
Flag}=4$ is assigned to redshifts with multiple good S/N line detections; a
${\rm Flag}=3.5$ is given to very good S/N single line detections; a ${\rm
Flag}=3$ is given to convincing single line detections. Lower ${\rm
Flag\,}(1{\rm\,and\,}2)$ spectra indicate redshifts that are not secure enough
for our purposes; ${\rm Flag}=-99$ are non-detections or failed reductions.
Examples of ${\rm Flag}=4,3.5,3$ spectra and redshifts are given in Figs. 3
and 4.

In a number of slits, more than one object was detected, either as a spatially
separate object or on the same line of sight, but with different redshifts. In
these cases multiple 1D spectra were extracted and analyzed. The correct
identification was attempted by inspection of the relevant images.

The procedure described above was performed independently by two of us (RPS
and RZ); discrepant assessments were discussed and resolved. We extracted 1119
spectra, of which 19 were not matched with an object from the photometric
parent catalogues. We matched 292 good spectra (${\rm Flag}\geq 3$): 163 in
the COSMOS field, 129 in the VVDS field. The complete statistics are given in
Table 1, where we list the numbers referring to primary spectra (targeting the
H$\alpha$ line) and secondary spectra (targeting the [O iii] or Pa lines).

Table 1: Statistics of observed spectra. Spectra | All |  $H$ band |  $K$ band | COSMOS |  $H$ band |  $K$ band | VVDS |  $H$ band |  $K$ band
---|---|---|---|---|---|---|---|---|---
Extracted | 1119 | 635 | 484 | 766 | 424 | 342 | 353 | 211 | 142
Good | 305 | 212 | 93 | 174 | 127 | 47 | 131 | 85 | 46
Identified | 1100 | 618 | 482 | 751 | 410 | 341 | 349 | 208 | 141
Good | 292 | 200 | 92 | 163 | 117 | 46 | 129 | 83 | 46
Primary | 851 | 446 | 405 | 597 | 316 | 281 | 254 | 130 | 124
Good | 249 | 158 | 91 | 139 | 94 | 45 | 110 | 64 | 46
Secondary | 249 | 172 | 77 | 154 | 94 | 60 | 95 | 78 | 17
Good | 43 | 42 | 1 | 24 | 23 | 1 | 19 | 19 | 0
Unidentified | 19 | 17 | 2 | 16 | 15 | 1 | 4 | 3 | 1
Good | 13 | 12 | 1 | 11 | 10 | 1 | 2 | 2 | 0
Primary | 14 | 12 | 2 | 11 | 10 | 1 | 3 | 2 | 1
Good | 8 | 7 | 1 | 7 | 6 | 1 | 1 | 1 | 0
Secondary | 5 | 5 | 0 | 4 | 4 | 0 | 1 | 1 | 0
Good | 5 | 5 | 0 | 4 | 4 | 0 | 1 | 1 | 0

Table 3 (column “Success Rate”) gives the number of extracted identified
spectra (a total of 1100) in each pointing together with the number of good
spectra $({\rm Flag}\geq 3)$ and the number of primary spectra collected. The
mean success rate (defined as the ratio of the number of identified good
spectra over the total number of collected identified spectra) is 0.27 (0.22
in the COSMOS field and 0.37 in the VVDS field; the lower success rate in the
COSMOS field stems from the suboptimal meteorological conditions under which
several COSMOS masks were observed). It is higher in the $H$ band (0.32; 0.28
in the COSMOS field and 0.40 in the VVDS field) than in the $K$ band (0.19;
0.13 in the COSMOS field and 0.33 in the VVDS field). The success rates
achieved by G2020 are better, which stems from the larger field of view (which
allowed an optimized choice of good candidates), the fixed wavelength range,
and the IFU available with the KMOS instrument. We investigate the properties
of the galaxies with unreliable spectra $({\rm Flag}<3)$ in Sect. 5.

The barycentric corrections $z_{\rm helcorr}=v_{\rm helcorr}/c$ appropriate to
each mask are listed in Table 3 together with the Julian date (JD) adopted for
the computation. This corresponds to the middle of the sequence of exposures.
When two series of exposures observed in different nights are summed together,
the JD refers to the first of the two. The barycentric corrections are
computed through the python routine pyals.helcorr from PyAstronomy; we quote
the two digits that affect the last quoted digit of the redshifts. Using the
relation $1+z_{\rm spec}=(1+z_{\rm meas})\,(1+z_{\rm helcorr})$, where $z_{\rm
meas}$ are the measured redshifts shown in Figs. 3 and 4, we compute the
redshifts $z_{\rm spec}$ given in Table 2 using the formula $z_{\rm
spec}=z_{\rm meas}+(1+z_{\rm meas})\,z_{\rm helcorr}$. In addition, Table 2
reports the object ID, its coordinates, the Flag, the line or ensemble of
lines used (H$\alpha$ plus possibly [N ii] and/or [S ii], [O iii] plus
possibly H$\beta$, Pa) and the name of the spectrum.

Figure 3: One- and two-dimensional spectra with ${\rm Flag}=4,3.5,3$ of
objects with $z_{\rm meas}<2$. The 2D spectra are 10 arcsec in width, with the
vertical scale given in pixels, and show the whole wavelength range (in
$\mu$m) observed. The 1D spectra show the wavelength range around the relevant
emission lines; the black solid lines show the measured flux (in arbitrary
units with a 3 pixel smoothing), the dotted lines the flux without smoothing
plus its errors, the red lines the sky (scaled down by a factor of 1000 and
shifted by $-0.2$ flux units). The vertical dashed lines indicate the emission
lines (with vacuum rest-frame wavelengths in Å) used (when visible) to measure
the spectroscopic redshift (not yet corrected to the heliocentric system).

Figure 3: continued.

Figure 4: One- and two-dimensional spectra with ${\rm Flag}=4$ and 3 of
objects with $z_{\rm meas}>2$. Lines as in Fig. 3.

A number of objects were observed multiple times, enabling an empirical
determination of the errors on our redshifts and to compare redshifts derived
from the $K$\- and $H$-band spectra. Figure 5 shows that the RMS uncertainty
on the redshifts of objects at $z<1.8$ with repeat observations is 0.0002, and
two times larger for objects with $z>1.8$. One COSMOS object $({\rm
ID}=481647)$ was observed by the previous C3R2 releases, providing $z_{\rm
spec}=1.501$, identical to $z_{\rm spec}=1.501$ obtained here. A further
COSMOS object $({\rm ID}=480046)$ was observed by Euclid Collaboration:
Stanford et al. (2021), who reported $z_{\rm spec}=2.2705$, while our
measurement is $z_{\rm spec}=2.2702$, in line with the results discussed
above. Following these findings, we quote the measured redshifts to four
decimal digits. The redshifts determined from H$\alpha$ and [O iii] lines
agree within the errors, with no appreciable bias.

A unique redshift $\langle z\rangle$ and flag were assigned to each object
with repeated observations by averaging the available measurements; the
resulting values are reported in Table 2 and used in the following figures.

Figure 5: Errors from repeated observations. The filled circles show the differences d$z$ between the spectroscopic redshifts determined from two or more spectra of the same objects using the H$\alpha$ line. If more than two spectra were collected, the difference to the average of the measurements is shown. The open circles show differences between redshifts based on the [O iii] lines; the open squares show differences between redshifts measured using the H$\alpha$ and the [O iii] lines. Table 2: Mean redshift and flag for objects with multiple spectra. Field | OBJ_ID | $\langle z\rangle$ |  $|\Delta z|/2$ or RMS | N | $\langle{\rm Flag}\rangle$ | Lines
---|---|---|---|---|---|---
COSMOS | 32961 | 1.4623 | 0.0003 | 2 | 3.75 | H$\alpha$
COSMOS | 38150 | 2.3945 | 0.0005 | 2 | 3.5 | H$\alpha$+[O iii]
COSMOS | 402635 | 2.1708 | 0.0005 | 2 | 3.5 | H$\alpha$+[O iii]
COSMOS | 462025 | 2.0875 | 0.0002 | 2 | 3 | [O iii]
COSMOS | 463893 | 2.3473 | 0 | 2 | 3.5 | H$\alpha$+[O iii]
COSMOS | 472716 | 1.7119 | 0.0001 | 2 | 3.25 | H$\alpha$
COSMOS | 479007 | 2.2725 | 0.0004 | 3 | 4 | H$\alpha$+[O iii]
COSMOS | 481315 | 2.4910 | 0.0003 | 2 | 4 | [O iii]
COSMOS | 481647 | 1.5010 | 0 | 2 | 4 | H$\alpha$
COSMOS | 484310 | 1.5879 | 0.0003 | 2 | 3.25 | H$\alpha$
COSMOS | 811438 | 2.3620 | 0.0003 | 2 | 3 | H$\alpha$
VVDS | 3324 | 1.5340 | 0.0001 | 2 | 4 | H$\alpha$
VVDS | 7941 | 1.5346 | 0 | 2 | 3.25 | H$\alpha$
VVDS | 22805 | 1.5333 | 0.0001 | 2 | 3.25 | H$\alpha$
VVDS | 24882 | 1.3763 | 0.0003 | 3 | 3.333 | H$\alpha$
VVDS | 24903 | 1.5781 | 0 | 2 | 3 | H$\alpha$
VVDS | 36412 | 1.5366 | 0 | 2 | 4 | H$\alpha$
VVDS | 37921 | 2.0007 | 0.0001 | 2 | 3.5 | [O iii]
VVDS | 140031 | 2.2141 | 0 | 2 | 3.5 | H$\alpha$+[O iii]
VVDS | 142226 | 1.5165 | 0 .0001 | 2 | 3.5 | H$\alpha$
VVDS | 144923 | 1.5600 | 0.0001 | 2 | 3.5 | H$\alpha$
VVDS | 160224 | 1.6061 | 0 | 3 | 3.667 | H$\alpha$
VVDS | 162982 | 2.2442 | 0.0007 | 2 | 4.0 | H$\alpha$+[O iii]
VVDS | 163515 | 1.5716 | 0.0001 | 3 | 3.5 | H$\alpha$
VVDS | 165659 | 2.1396 | 0.0001 | 2 | 3.5 | H$\alpha$+[O iii]
VVDS | 165940 | 2.2649 | 0.0002 | 2 | 3.5 | H$\alpha$
VVDS | 167263 | 2.2599 | 0.0002 | 2 | 3.5 | H$\alpha$
VVDS | 167264 | 2.2591 | 0.001 | 2 | 3 | [O iii]
VVDS | 168107 | 1.5599 | 0.0003 | 2 | 3 | H$\alpha$
VVDS | 168869 | 2.4433 | 0.0004 | 2 | 3.5 | H$\alpha$+[O iii]
VVDS | 171656 | 2.2376 | 0.0001 | 2 | 3 | H$\alpha$+[O iii]
VVDS | 179905 | 2.0605 | 0.0003 | 2 | 4 | H$\alpha$
VVDS | 179990 | 2.0356 | 0 | 2 | 3 | H$\alpha$
VVDS | 383107 | 2.1861 | 0 | 2 | 3 | H$\alpha$+[O iii]
VVDS | 515718 | 2.3259 | 0.0003 | 2 | 3 | H$\alpha$+[O iii]

##  5 Results

We measured good $({\rm Flag}\geq 3)$ spectroscopic redshifts for 253 objects
(two of which already known): 71 with ${\rm Flag}=4$, 62 with ${\rm
Flag}=3.5$, and 120 with ${\rm Flag}=3$. Figure 6 compares these to the
photometric (left) and the SOM-based (right) redshifts. The photometric
redshifts are from Ilbert et al. (2006) and Laigle et al. (2016); the SOM-
based redshifts are the averages of the photometric redshifts of the galaxies
belonging to the SOM cell. There are no catastrophic failures with $|z_{\rm
phot}-z_{\rm spec}|/(1+z_{\rm spec})\geq 0.15$ and ${\rm Flag}\geq 3$. Seven
objects have $|z_{\rm phot,SOM}-z_{\rm spec}|/(1+z_{\rm spec})\geq 0.15$; we
examine the cells they belong to below. The values of $\sigma_{NMAD}=1.48{\rm
Median}(|z-z_{\rm spec}|/(1+z_{\rm spec}))$ and ${\rm Bias}={\rm
Mean}((z-z_{\rm spec})/(1+z_{\rm spec})))$ are comparable to what achieved in
previous C3R2 releases; for example G2020 quote $\sigma_{NMAD}=0.03$ and ${\rm
Bias}=-0.003$ when considering $z=z_{\rm phot}$ and $\sigma_{NMAD}=0.044$ and
${\rm Bias}=0.027$ when considering $z=z_{\rm phot,SOM}$.

Figure 6 shows that the agreement between photometric and spectroscopic
redshifts for objects with $z_{\rm spec}<2$ is excellent, with a mean
difference of $-0.006$ and ${\rm RMS}=0.03$. At higher redshift, however,
photometric redshifts appear systematically larger, with $\langle(z_{\rm
phot}-z_{\rm spec})/(1+z_{\rm spec})\rangle=0.02$ and similar RMS. We
investigate this issue by examining the whole C3R2 dataset published to date
(see Fig. 7). When averaged in redshift bins of width 0.1, the mean difference
$\langle(z_{\rm phot}-z_{\rm spec})/(1+z_{\rm spec})\rangle$ appears slightly
negative ($\approx-0.01\pm 0.0015$) up to redshifts 1.7, and slightly positive
($\approx+0.01\pm 0.003$) at higher redshifts, consistently in all datasets
and for both ${\rm Flag}\geq 3$ or ${\rm Flag}=4$ redshifts. Moreover, in each
bin up to redshift 1.7 the mean difference, or bias, is well determined with a
signal-to-noise ratio S/N between 3 and 8. This S/N is lower (between 2 and 6)
at redshifts higher than 2; the bias is unconstrained (with S/N less than 1)
in between. The S/N improvement in each bin achieved by the new redshifts
released here is $\leq 0.5$.

This shows that the C3R2 project is able to detect and correct the residual
small biases present in the most accurate available photometric redshift
samples that can be used as reference in the Euclid mission. Therefore the
tight Euclid requirement that the mean redshift in each tomographic bin must
be constrained at the level of $0.002(1+z)$ is achieved up to redshift 1.7
thanks to the calibration provided by the C3R2 dataset. It is almost achieved
for redshifts higher than 2, but remains problematic in between, where the
error on the possible residual bias is $\approx 0.005$.

How the spectroscopic calibration of single SOM cells will be implemented when
building the lensing tomographic bins for Euclid is still under investigation
and goes beyond the scope of this paper.

Figure 6: Comparison between photometric and spectroscopic redshifts. Left:
Comparison between $z_{\rm phot}$ and $z_{\rm spec}$ for high-quality $({\rm
Flag}\geq 3)$ redshift galaxies observed during the LBT campaign. Crosses show
spectroscopic redshifts determined from the H$\alpha$ line, circles with
crosses from the [O iii] lines. The dotted lines define the region outside
which the $z_{\rm phot}$ is considered a catastrophic failure, defined by a
redshift error $|z_{\rm phot}-z_{\rm spec}|/(1+z_{\rm spec})\geq 0.15$. Right:
Same as the left panel, but comparing $z_{\rm phot,SOM}$ and $z_{\rm spec}$.
The values of $\sigma_{NMAD}=1.48{\rm Median}(|z-z_{\rm spec}|/(1+z_{\rm
spec}))$ and ${\rm Bias}={\rm Mean}((z-z_{\rm spec})/(1+z_{\rm spec})))$ are
also given, with $z=z_{\rm phot}$ in the left plot and $z=z_{\rm phot,SOM}$ in
the right.

Figure 7: Mean differences between photometric and spectroscopic redshifts.
Left: Mean differences of $(z_{\rm phot}-z_{\rm spec})/(1+z_{\rm spec})$ of
non-catastrophic failures in bins of $z_{\rm spec}$ as a function of $z_{\rm
spec}$ for ${\rm Flag}\geq 3$ redshifts released by the C3R2 project: yellow
from Masters et al. (2015, 2017, 2019); magenta from G2020; red from Euclid
Collaboration: Stanford et al. (2021); blue, this paper. The black line shows
the average in bins of the whole sample, the dotted lines the error range.
Right: Same, but for ${\rm Flag}=4$ redshifts.

Figure 6, right shows that six galaxies have $|z_{\rm phot,SOM}-z_{\rm
spec}|/(1+z_{\rm spec})>0.15$. A seventh galaxy at $z_{\rm phot,SOM}=0.8$ (and
therefore not visible in the figure) has a similarly discrepant redshift. As
noted in G2020, they belong to cells with a large spread in photometric
redshifts, probing the second peak of the distribution or its tail (see Fig.
8).

Figure 8: Histogram of $z_{\rm phot}$ of galaxies populating each cell with
$|z_{\rm phot,SOM}-z_{\rm spec}|/(1+z_{\rm spec})>0.15$ (right panel of Fig.
6). The distribution is normalized by dividing the number of galaxies in each
$z_{\rm phot}$ bin by the total number of $z_{\rm phot}$ populating the
considered cell; the number is indicated by the letter N in the top left
panel, and written in the same position in the others. Similarly, the cell
number (CellID) is also given in each panel. The $z_{\rm phot,SOM}$ is
represented by the dashed line, whereas dotted lines indicate $z_{\rm spec}$
measured during our program. The horizontal bar centered on the mean $z_{\rm
phot}$ is the RMS of the histogram.

Figure 9 examines the success rate as a function of redshift. As already
discussed above, the success rate is lower in the $K$ band and peaks when the
redshifted H$\alpha$ line is around the mid-redshift of either band. This is
expected since the wavelength coverage depends upon the position of the
galaxies on the masks, and we set the central wavelength of the spectrographs
to the average of the expected H$\alpha$ positions. Moreover, the focus of the
spectrographs deteriorates for objects that are not within the central 2.8
arcmin stripe of the field. Similarly, the [O iii] lines at $z_{\rm phot}\leq
2.1$ fall outside of the covered wavelength range in the $H$ band if the
objects are not in extreme positions on the masks. Overall, the success rate
achieved for $z_{\rm phot}\geq 2.0$ objects targeting the H$\alpha$ in the $K$
band or the [O iii] lines in the $H$ band is similar. In contrast, we managed
to detect only once (with ${\rm Flag}=3$) the Pa lines from the 77 targeted
$z_{\rm phot}\leq 1.7$ objects in the $K$ band. However, these objects were
selected as fillers when space was available in the masks and no H$\alpha$
targets were left. Figure 10 examines the success rate as a function of the
apparent total $H$-band magnitude of the galaxies. This is not a strong
function of the $H$ magnitude; it is approximately 35%, down to $H$ magnitudes
of 23 and declining for fainter objects.

Figure 9: Spectroscopic success rate as a function of redshift.Top: Histogram
of $z_{\rm phot}$ of targeted galaxies (dashed lines), targeting H$\alpha$
(solid lines), and the [O iii] or Pa lines (dotted lines). Bottom: Success
rate as a function of $z_{\rm phot}$ considering all lines (H$\alpha$, [O
iii], Pa, full line), based on H$\alpha$ only (dotted line), or on [O iii] or
Pa (dashed line). Figure 10: Spectroscopic success rate as a function of
magnitude. Top: Histogram of the observed $H$ total magnitudes for all
observed targets (dotted line), for secondary targets (long-dashed line), and
for those with high-quality spectroscopic redshifts (full line). Bottom:
Success rate as a function of $H$ total magnitudes over the whole probed
redshift range (full line), and split according to band (dotted: $H$ band or
$1.3<z_{\rm phot}<1.7$; dashed: $K$ band, or $2<z_{\rm phot}<2.7$. The long-
dashed line shows the success rate targeting the [O iii] line.

With the same motivation as in G2020, we now examine the success rate in
populating SOM cells with spectra. We targeted 518 cells (388 in the COSMOS
field, 194 in the VVDS field, with overlap), obtaining reliable spectra $({\rm
Flag}\geq 3)$ for 202 (127 in COSMOS, 94 in VVDS with overlap), translating to
a success rate of 39% (33% in COSMOS, 48% in VVDS). Of the 202 cells probed
successfully here, 49 were empty before these observations; for the remaining
153 cells with at least one good spectroscopic redshift from previous C3R2
campaigns, on average our observations increased the number of spectroscopic
redshifts per cell by 72%.

Figure 11 shows the distribution of the SOM cells probed by the current
spectroscopic release, together with the cells still empty. Summing up the
contributions of all C3R2 releases, we find the following. In the 839 cells
with $1.3<z_{\rm phot,SOM}<1.7$, there are 52491 galaxies (with I-band
magnitudes brighter than 24.5 in the COSMOS and VVDS fields). In 683 of these
cells (81%), where 45370 galaxies are found (86% of the total), we collected
at least one good spectroscopic redshift. In the 895 cells with $2<z_{\rm
phot,SOM}<2.7$, there are 40013 galaxies. In 683 of these cells (74%), where
30981 galaxies are found (77% of the total), we collected at least one good
spectroscopic redshift.

Figure 11: Cells probed by the current spectroscopic release (filled squares)
and cells still lacking spectroscopy (empty squares). Blue cells have
$1.3<z_{\rm phot,SOM}<1.7$, black cells have $1.7<z_{\rm phot,SOM}<2.0$, and
red cells have $2.0<z_{\rm phot,SOM}<2.7$. Open circles are the 49 cells
without spectroscopy before this release. The circles without a centered
square have $z_{\rm phot,SOM}$ outside the probed range.

##  6 Discussion and conclusions

We present the results of the LBT campaign to calibrate photometric redshifts
in the redshift range 1.3 to 2.7 using the LUCI near-infrared spectrographs in
the framework of the C3R2 project. We observed 88 masks, 58 in the COSMOS
field and 30 in the VVDS field, with an average of 12 objects per mask, aiming
to detect the H$\alpha$ line for primary targets, and the [O iii] or Pa lines
for secondary objects. We extracted 1119 spectra, 1100 of which were
identified as C3R2 galaxies. From 292 of these galaxies we were able to
measure reliable spectroscopic redshifts. We assessed their precision from
repeated measurements to be in the range $\Delta z\sim 0.0002$ to 0.0004.
After averaging repeat measurements, we ended up with reliable spectroscopic
redshifts for 253 galaxies, two of which with already-known values.

Comparison with the C3R2 photometric redshifts shows that none of these
galaxies are catastrophic outliers. The values of $\sigma_{\rm NMAD}$ and the
bias are comparable to those reported in the previous C3R2 releases. Analyzing
the whole C3R2 spectroscopic database published to date, we detect a small
systematic shift $\langle(z_{\rm phot}-z_{\rm spec})/(1+z_{\rm spec})\rangle$
on the order of $-0.01\pm 0.0015$ in the redshift range $1.3<z_{\rm phot}<1.8$
and of $+0.01\pm 0.003$ in the range $2<z_{\rm phot}<2.7$. This is relevant
for the calibration of the redshifts of SOM cells in these redshift ranges,
essentially matching the Euclid requirement of knowing the mean redshift of
each tomografic bin to $0.002(1+z)$. Our redshift determinations populate 49
SOM cells with no prior spectroscopic measurements, approximately doubling the
occupation numbers of an additional 153 cells. Seven SOM cells have $|z_{\rm
phot,SOM}-z_{\rm spec}|/(1+z_{\rm spec})\geq 0.15$; they have a large spread
in photometric redshifts, and our objects probe the second peak of the
distribution or its tail.

In the redshift range 1.3 to 1.7 there are still 156 cells (19%) without at
least one good spectroscopic redshift; in these cells that lack a
spectroscopic calibration we find only 14% of the galaxy population. In the
redshift range 2 to 2.7 there are 232 cells (26%) without at least one good
spectroscopic redshift; in these cells we find 23% of the galaxy population.
In between, in the redshift range 1.7 and 2 where telluric absorption makes
the direct observation of H$\alpha$ impossible, the number of cells without at
least one good spectroscopic redshift is 126 (28%); in these cells we find 26%
of the galaxy population with redshifts between 1.7 and 2. The redshift bias
$\langle(z_{\rm phot}-z_{\rm spec})/(1+z_{\rm spec})\rangle$ is not well
constrained, with an error (0.005) larger than the Euclid requirement.

Two questions arise. First, is it worth attempting to calibrate the missing
cells in the $H$ and $K$ bands with LUCI at the LBT? Probably not, since their
density is too low for the field of view available. Moreover, G2020 found that
most of them have low star formation rates, making the detection of emission
lines very difficult, and the success rate (around 30%) of the present
campaign is not particularly encouraging. Second, is it worth attempting the
calibration of the cells missing in the redshift range 1.7 to 2 with ground-
based facilities? Detecting the H$\gamma$, H$\beta$, and [O iii] lines in the
$J$ band up to redshift 2, 1.9, and 1.8, respectively, could be possible with
an increasing probability of success. Whether the LBT with the LUCI
spectrographs should be used for such a campaign depends on the density on the
sky of the objects needing spectra. However, the difficult remaining sources
at these redshifts are primarily passive galaxies, and so spectroscopic
searches for Balmer and [O iii] emission lines are unlikely to be efficient or
successful. A costly solution could be ground-based (optical) absorption-line
spectroscopy. A release of optical spectra gathered at the VLT and the
GRANTECAN telescopes is in preparation. In the end the (possibly partial)
natural solution will come from Euclid itself: its spectroscopic program will
deliver near-infrared spectra in the relevant redshift range free of telluric
absorption. The survey is designed to detect emission lines down to $2\times
10^{-16}{\rm ergs}^{-1}{\rm cm}^{-2}$ at $3.5\sigma$ in the wide
configuration, and reach up to 2 mag fainter levels in the deep fields (Euclid
Collaboration: Scaramella et al., 2021), or $3$ to $6\times 10^{-17}{\rm
ergs}^{-1}{\rm cm}^{-2}$. Using the H$\alpha$ fluxes measured by G2020, we
estimate that 60 to 90% of the sources will be detected within these limits in
the deep fields. Therefore, the mission itself will provide enough spectra to
finish the photometric redshift calibration in the near-infrared range to the
required precision. In particular, a question that needs to be clarified is
whether in a given SOM cell the galaxies for which we are able or unable to
measure a spectroscopic redshift might have different redshift distributions.

###### Acknowledgements.

The Euclid Consortium acknowledges the European Space Agency and a number of
agencies and institutes that have supported the development of Euclid, in
particular the Academy of Finland, the Agenzia Spaziale Italiana, the Belgian
Science Policy, the Canadian Euclid Consortium, the French Centre National
d’Etudes Spatiales, the Deutsches Zentrum für Luft- und Raumfahrt, the Danish
Space Research Institute, the Fundação para a Ciência e a Tecnologia, the
Ministerio de Ciencia e Innovación, the National Aeronautics and Space
Administration, the National Astronomical Observatory of Japan, the
Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, the
Romanian Space Agency, the State Secretariat for Education, Research and
Innovation (SERI) at the Swiss Space Office (SSO), and the United Kingdom
Space Agency. A complete and detailed list is available on the Euclid web site
(http://www.euclid-ec.org). RS, MF, VG, RB acknowledge support by the
Deutsches Zentrum für Luft- und Raumfahrt (DLR) grant 50 QE 1101. The work of
DS was carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. We thank the staff of the LBT
observatory for their support during the mask preparation and the execution of
the observations.

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##  Appendix A Table A.1

Table 3: List of the observed masks. Field | Mask ID |  RAcen |  Deccen | Rot.Angle | nExp | UT Date | JD | $z_{\rm helcorr}$ | Success Rate
---|---|---|---|---|---|---|---|---|---
|  | (hms) | (dms) | (deg) |  $(\times 200\,{\rm s}$) | (yyyy.mm.dd) |  | $(\times 10^{5})$ | $({\rm Flag}\geq 3/{\rm Prim}/{\rm Obs})$
VVDS | M1H | 022614.372 | $-045554.320$ | 15 | 36 | 2019-10-03 | 2458759.83 | 3.6 | 6/12/14
VVDS | M2H | 022622.493 | $-045356.990$ | 20 | 36 | 2019-10-03 | 2458759.95 | 3.5 | 7/8/12
VVDS | M3H | 022622.572 | $-045759.610$ | $-16$ | 36 | 2019-10-07 | 2458763.80 | 3.0 | 4/7/12
VVDS | M4H | 022606.238 | $-045557.250$ | 0 | 36 | 2019-10-07 | 2458764.93 | 2.7 | 4/10/14
VVDS | M5H | 022630.656 | $-044152.010$ | 75 | 36 | 2019-10-09 | 2458765.82 | 2.7 | 7/7/12
VVDS | M9H | 022550.162 | $-045358.310$ | 50 | 22 | 2020-01-19 | 2458867.75 | $-9.7$ | 6/9/13
VVDS | M9K | 022550.162 | $-045358.310$ | 50 | 23 | 2020-01-19 | 2458867.75 | $-9.7$ | 1/6/7
VVDS | M12K | 022437.840 | $-041546.890$ | 145 | 26 | 2020-01-23 | 2458871.61 | $-9.7$ | 0/6/7
COSMOS | M1H | 095839.234 | +015608.340 | 160 | 36 | 2020-03-16 | 2458924.65 | $-3.9$ | 6/13/16
COSMOS | M1K | 095839.234 | +015608.340 | 160 | 36 | 2020-03-16 | 2458924.65 | $-3.9$ | 2/11/13
COSMOS | M2H | 100024.224 | +021252.150 | $-10$ | 33 | 2020-03-16 | 2458924.85 | $-4.0$ | 1/6/7
COSMOS | M2K | 100024.224 | +021252.150 | $-10$ | 33 | 2020-03-16 | 2458924.85 | $-4.0$ | 0/4/7
COSMOS | M3H | 095856.377 | +020807.150 | 135 | 36 | 2020-03-17 | 2458925.65 | $-4.0$ | 6/12/14
COSMOS | M3K | 095856.377 | +020807.150 | 135 | 36 | 2020-03-17 | 2458925.65 | $-4.0$ | 1/8/12
VVDS | M6H_1 | 022726.448 | $-045159.520$ | $-105$ | 25 | 2020-10-03 | 2459125.32 | 3.5 | 4/7/12
VVDS | M6K_1 | 022726.448 | $-045159.520$ | $-105$ | 25 | 2020-10-03 | 2459125.32 | 3.5 | 2/10/11
VVDS | M7H | 022445.672 | $-040142.190$ | 195 | 35 | 2020-10-03 | 2459125.46 | 3.6 | 4/3/12
VVDS | M7K | 022445.672 | $-040142.190$ | 195 | 35 | 2020-10-03 | 2459125.46 | 3.6 | 4/14/15
VVDS | M8H | 022631.827 | $-043805.980$ | 240 | 36 | 2020-10-04 | 2459126.30 | 3.3 | 4/6/11
VVDS | M8K | 022631.827 | $-043805.980$ | 240 | 36 | 2020-10-04 | 2459126.30 | 3.3 | 4/6/9
VVDS | M10H | 022534.064 | $-040945.080$ | 170 | 36 | 2020-10-04 | 2459126.45 | 3.4 | 4/11/14
VVDS | M10K | 022534.064 | $-040945.080$ | 170 | 36 | 2020-10-04 | 2459126.45 | 3.4 | 3/8/13
VVDS | M12H | 022437.840 | $-041546.890$ | 145 | 36 | 2020-10-05 | 2459127.46 | 3.2 | 5/6/12
VVDS | M12K | 022437.840 | $-041546.890$ | 145 | 36 | 2020-10-06 | 2459127.46 | 3.2 | 6/11/11
VVDS | M11H | 022526.034 | $-043954.090$ | 335 | 36 | 2020-10-05 | 2459127.59 | 3.3 | 5/7/12
VVDS | M11K | 022526.034 | $-043954.090$ | 335 | 36 | 2020-10-05 | 2459127.59 | 3.3 | 5/11/11
VVDS | M13H | 022429.716 | $-044355.300$ | 340 | 36 | 2020-10-06 | 2459128.38 | 3.0 | 5/8/11
VVDS | M13K | 022429.716 | $-044355.300$ | 340 | 37 | 2020-10-06 | 2459128.38 | 3.0 | 5/10/10
VVDS | M14H_1 | 022630.358 | $-043954.870$ | 70 | 11 | 2020-10-06 | 2459128.50 | 3.1 | 5/5/9
VVDS | M14K_1 | 022630.358 | $-043954.870$ | 70 | 11 | 2020-10-06 | 2459128.50 | 3.1 | 8/11/11
VVDS | M14H_2 | 022630.358 | $-043954.870$ | 70 | 30 | 2020-10-07 | 2459128.50 | 3.1 | summed to M14H_1
VVDS | M14K_2 | 022630.358 | $-043954.870$ | 70 | 27 | 2020-10-07 | 2459128.50 | 3.1 | summed to M14K_1
VVDS | M4H | 022606.238 | $-045557.250$ | 0 | 36 | 2020-10-07 | 2459129.44 | 3.0 | 4/10/14
VVDS | M4K | 022606.238 | $-045557.250$ | 0 | 36 | 2020-10-07 | 2459129.44 | 3.0 | 2/9/13
VVDS | M3H | 022622.572 | $-045759.610$ | $-16$ | 36 | 2020-10-04 | 2459130.31 | 2.7 | 3/7/12
VVDS | M3K | 022622.572 | $-045759.610$ | $-16$ | 36 | 2020-10-04 | 2459130.31 | 2.7 | 1/10/11
VVDS | M6H_0 | 022726.448 | $-045159.520$ | $-105$ | 3 | 2020-10-07 | 2459125.32 | 3.5 | summed to M6H_1
VVDS | M6K_0 | 022726.448 | $-045159.520$ | $-105$ | 3 | 2020-10-07 | 2459125.32 | 3.5 | summed to M6K_1
VVDS | M5H | 022630.656 | $-044152.010$ | 75 | 33 | 2020-10-08 | 2459130.46 | 2.8 | 6/7/12
VVDS | M5K | 022630.656 | $-044152.010$ | 75 | 33 | 2020-10-08 | 2459130.46 | 2.8 | 5/12/12
COSMOS | M7H | 100016.331 | +023959.780 | 145 | 36 | 2020-12-20 | 2459203.97 | 8.8 | 3/7/10
COSMOS | M7K | 100016.331 | +023959.780 | 145 | 37 | 2020-12-20 | 2459203.97 | 8.8 | 0/7/8
COSMOS | M6H | 100200.465 | +024022.660 | 180 | 36 | 2020-12-21 | 2459204.90 | 8.8 | 8/14/18
COSMOS | M6K | 100200.465 | +024022.660 | 180 | 36 | 2020-12-21 | 2459204.90 | 8.8 | 2/10/17
COSMOS | M8H | 100057.749 | +024042.990 | 55 | 30 | 2020-12-21 | 2459205.03 | 8.7 | 5/12/14
COSMOS | M8K | 100057.749 | +024042.990 | 55 | 30 | 2020-12-21 | 2459205.03 | 8.7 | 0/9/10
COSMOS | M10H | 095928.310 | +023020.540 | 70 | 28 | 2020-12-22 | 2459205.53 | 8.7 | 5/11/16
COSMOS | M10K | 095928.310 | +023020.540 | 70 | 28 | 2020-12-22 | 2459205.53 | 8.7 | 2/4/7
COSMOS | M9H | 095936.806 | +023227.230 | 230 | 35 | 2020-12-22 | 2459205.90 | 8.7 | 5/8/11
COSMOS | M9K | 095936.806 | +023227.230 | 230 | 36 | 2020-12-22 | 2459205.90 | 8.7 | 6/10/12
COSMOS | M11H | 095953.706 | +024016.910 | 145 | 36 | 2021-01-14 | 2459228.81 | 6.1 | 3/11/15
COSMOS | M11K | 095953.706 | +024016.910 | 145 | 36 | 2021-01-14 | 2459228.81 | 6.1 | 2/8/13
COSMOS | M12H | 100144.876 | +021013.710 | 175 | 36 | 2021-01-15 | 2459229.82 | 6.0 | 5/11/15
COSMOS | M12K | 100144.876 | +021013.710 | 175 | 36 | 2021-01-15 | 2459229.82 | 6.0 | 0/5/7
COSMOS | M13H | 100112.552 | +014557.890 | 85 | 36 | 2021-01-15 | 2459229.93 | 6.0 | 5/10/11
COSMOS | M7H | 100016.331 | +023959.780 | 145 | 36 | 2021-01-16 | 2459230.83 | 5.8 | 3/7/10
COSMOS | M7K | 100016.331 | +023959.780 | 145 | 36 | 2021-01-16 | 2459230.83 | 5.8 | 5/10/11
COSMOS | M8H | 100200.465 | +024022.660 | 180 | 40 | 2021-01-16 | 2459269.20 | 5.7 | 4/10/14
COSMOS | M8K | 100200.465 | +024022.660 | 180 | 40 | 2021-01-16 | 2459269.20 | 5.7 | 2/12/13
COSMOS | M14H | 100135.484 | +022000.480 | 160 | 36 | 2021-02-20 | 2459265.25 | 0.2 | 2/11/14
COSMOS | M14K | 100135.484 | +022000.480 | 160 | 37 | 2021-02-20 | 2459265.25 | 0.2 | 0/8/12
COSMOS | M15H | 100145.151 | +024022.550 | 115 | 36 | 2021-02-23 | 2459268.38 | $-0.3$ | 3/14/17
COSMOS | M15K | 100145.151 | +024022.550 | 115 | 36 | 2021-02-23 | 2459268.38 | $-0.3$ | 3/14/15
COSMOS | M17H | 100112.883 | +022431.600 | 140 | 36 | 2021-02-23 | 2459268.23 | $-0.4$ | 6/14/17
COSMOS | M17K | 100112.883 | +022431.600 | 140 | 37 | 2021-02-23 | 2459268.23 | $-0.4$ | 2/16/16
COSMOS | M18H | 100120.693 | +022216.430 | 105 | 27 | 2021-02-23 | 2459269.20 | $-0.5$ | 4/12/14
COSMOS | M18K | 100120.693 | +022216.430 | 105 | 27 | 2021-02-24 | 2459269.20 | $-0.5$ | 0/7/10
COSMOS | M20H | 100016.511 | +014607.640 | 150 | 36 | 2021-02-24 | 2459269.30 | $-0.5$ | 5/11/14
COSMOS | M20K | 100016.511 | +014607.640 | 150 | 36 | 2021-02-24 | 2459269.30 | $-0.5$ | 4/9/13
COSMOS | M22H | 095944.102 | +022014.340 | 30 | 31 | 2021-02-24 | 2459269.41 | $-0.5$ | 1/10/15
COSMOS | M22K | 095944.102 | +022014.340 | 30 | 32 | 2021-02-24 | 2459269.41 | $-0.5$ | 1/15/18
Table 1: continued. Field | Mask ID |  RAcen |  Deccen | Rot.Angle | nExp | UT Date | JD | $z_{\rm helcorr}$ | Success Rate
---|---|---|---|---|---|---|---|---|---
|  | (hms) | (dms) | deg | $(\times 200\,{\rm s})$ | (yyy.mm.dd) |  | $(\times 10^{5})$ | $({\rm Flag}\geq 3/{\rm Prim}/{\rm Observed})$
COSMOS | M23H | 095912.153 | +015008.170 | 90 | 23 | 2021-03-21 | 2459294.15 | $-4.6$ | 3/11/15
COSMOS | M23K | 095912.153 | +015008.170 | 90 | 23 | 2021-03-21 | 2459294.15 | $-4.6$ | 1/8/12
COSMOS | LAE3H | 100025.092 | +021627.160 | 0 | 19 | 2021-03-22 | 2459295.19 | $-4.7$ | 0/6/6
COSMOS | LAE3K | 100025.092 | +021627.160 | 0 | 19 | 2021-03-22 | 2459295.19 | $-4.7$ | 0/4/5
COSMOS | LAE4H | 100041.352 | +021239.210 | $-15$ | 36 | 2021-03-23 | 2459296.18 | $-4.9$ | 0/3/6
COSMOS | LAE4K | 100041.352 | +021239.210 | $-15$ | 36 | 2021-03-23 | 2459296.18 | $-4.9$ | 3/6/10
COSMOS | M24H | 100153.446 | +021613.970 | 100 | 15 | 2021-03-23 | 2459296.26 | $-4.8$ | 0/9/15
COSMOS | M24K | 100153.446 | +021613.970 | 100 | 15 | 2021-03-23 | 2459296.26 | $-4.8$ | corrupted
COSMOS | M25H | 095936.030 | +020806.570 | 180 | 13 | 2021-03-27 | 2459301.35 | $-5.5$ | 1/12/17
COSMOS | M25K | 095936.030 | +020806.570 | 180 | 13 | 2021-03-27 | 2459301.35 | $-5.5$ | 0/17/17
COSMOS | M25H | 095936.030 | +020806.570 | 180 | 36 | 2021-04-20 | 2459324.24 | $-8.1$ | 7/12/17
COSMOS | M25K | 095936.030 | +020806.570 | 180 | 36 | 2021-04-20 | 2459324.24 | $-8.1$ | 4/17/17
COSMOS | M28H | 095952.615 | +015207.480 | 150 | 35 | 2021-04-24 | 2459328.19 | $-8.5$ | 7/14/14
COSMOS | M28K | 095952.615 | +015207.480 | 150 | 35 | 2021-04-24 | 2459328.19 | $-8.5$ | 1/14/14
COSMOS | M27H_1 | 095912.104 | +022214.200 | 140 | 16 | 2021-04-22 | 2459328.28 | $-8.5$ | 6/13/14
COSMOS | M27H_2 | 095912.104 | +022214.200 | 140 | 16 | 2021-04-23 | 2459328.28 | $-8.5$ | summed to M27H_1
COSMOS | M27K_1 | 095912.104 | +022214.200 | 140 | 16 | 2021-04-22 | 2459328.28 | $-8.5$ | corrupted
COSMOS | M27K_2 | 095912.104 | +022214.200 | 140 | 16 | 2021-04-23 | 2459328.28 | $-8.5$ | 2/6/10
COSMOS | M29H | 095912.178 | +021414.250 | 15 | 36 | 2021-04-25 | 2459329.20 | $-8.6$ | 4/11/13
COSMOS | M29K | 095912.178 | +021414.250 | 15 | 36 | 2021-04-25 | 2459329.20 | $-8.6$ | 2/13/13
COSMOS | M24H | 100153.446 | +021613.970 | 100 | 10 | 2021-04-25 | 2459329.28 | $-8.5$ | 4/9/15
COSMOS | M24K | 100153.446 | +021613.970 | 100 | 10 | 2021-04-25 | 2459329.28 | $-8.5$ | 1/14/14
COSMOS | M19H | 100104.598 | +014801.750 | 135 | 32 | 2021-05-19 | 2459328.28 | $-9.6$ | 4/12/15
COSMOS | M19K | 100104.598 | +014801.750 | 135 | 34 | 2021-05-19 | 2459328.28 | $-9.6$ | 0/15/15

##  Appendix B Table B.1

Table 2: Sample of galaxies with good spectroscopic redshifts. The explanation of the different columns is given in Sect. 4.  OBJ_ID | RA | Dec | $z_{\rm spec}$ | Flag | Line | 1D-Spectrum
---|---|---|---|---|---|---
13275 | 150.3162252 | 1.7379527 | 2.4078 | 4.0 |  [O iii] | COSMOS_LBT_JAN21_1d_13275_M13Hsky_S21
20825 | 150.0527463 | 1.7531398 | 1.6520 | 4.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_20825_M20Hsky_S08
21075 | 150.2729757 | 1.7538638 | 1.5172 | 3.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_21075_M13Hsky_S13
21964 | 150.0395616 | 1.7555454 | 2.5610 | 3.0 |  [O iii] | COSMOS_LBT_FEB21_1d_21964_M20Hsky_S19
26585 | 150.079045 | 1.7650675 | 2.3980 | 4.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_26585_M20Ksky_S16
28028 | 150.3115341 | 1.7680673 | 1.5573 | 3.5 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_28028_M13Hsky_S17
31318 | 150.0632315 | 1.7735528 | 2.2090 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_31318_M20Ksky_S11
31613 | 150.2616012 | 1.7747734 | 2.2790 | 4.0 |  [O iii] | COSMOS_LBT_MAY21_1d_31613_M19Hsky_S17
32792 | 150.0340033 | 1.7783992 | 2.3520 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_32792_M20Ksky_S14
32961 | 150.281817 | 1.778883 | 1.4621 | 4.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_32961_M13Hsky_S14
32961 | 150.281817 | 1.778883 | 1.4626 | 3.5 |  H$\alpha$ | COSMOS_LBT_MAY21_1d_32961_M19Hsky_S08
33981 | 150.0619008 | 1.7806075 | 1.6460 | 4.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_33981_M20Hsky_S17
34952 | 150.2745122 | 1.7830993 | 1.4406 | 3.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_34952_M13Hsky_S12
35658 | 150.0938201 | 1.7841196 | 1.4990 | 4.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_35658_M20Hsky_S12
38008 | 150.2506447 | 1.7882888 | 1.5028 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAY21_1d_38008_M19Hsky_S18
38150 | 150.0593597 | 1.788839 | 2.3940 | 4.0 |  [O iii] | COSMOS_LBT_FEB21_1d_38150_M20Hsky_S21
38150 | 150.0593597 | 1.788839 | 2.3950 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_38150_M20Ksky_S13
51484 | 149.7970089 | 1.8136581 | 1.6334 | 3.5 |  H$\alpha$ | COSMOS_LBT_MAR21_1d_51484_M23Hsky_S15
53612 | 149.7731289 | 1.8199504 | 1.5079 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR21_1d_53612_M23Hsky_S13
55494 | 150.292338 | 1.8234505 | 1.3193 | 4.0 |  H$\alpha$ | COSMOS_LBT_MAY21_1d_55494_M19Hsky_S09
63116 | 149.9518298 | 1.8386457 | 1.6518 | 3.5 |  H$\alpha$ | COSMOS_LBT_APR21_1d_63116_M28Hsky_S21
63265 | 149.9568087 | 1.8382493 | 1.6498 | 4.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_63265_M28Hsky_S09
63462 | 149.9680223 | 1.8398813 | 1.6498 | 3.5 |  H$\alpha$ | COSMOS_LBT_APR21_1d_63462_M28Hsky_S10
63645 | 149.7895905 | 1.8398429 | 1.4849 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR21_1d_63645_M23Hsky_S14
71209 | 149.7748281 | 1.8565425 | 2.5118 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR21_1d_71209_M23Ksky_S13
72589 | 149.9614682 | 1.860202 | 1.5558 | 4.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_72589_M28Hsky_S20
72810 | 150.0038562 | 1.8537445 | 2.5107 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_72810_M28Ksky_S09
76300 | 149.9797066 | 1.8673859 | 1.4198 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_76300_M28Hsky_S08
76722 | 149.9897509 | 1.8677315 | 1.3573 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_76722_M28Hsky_S15
91047 | 149.9912965 | 1.8967987 | 1.4948 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_91047_M28Hsky_S16
100154 | 149.6682826 | 1.915744 | 1.4394 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_100154_M1Hsky_S09
109400 | 149.6567535 | 1.9354134 | 1.6336 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_109400_M1Hsky_S12
110669 | 149.6868649 | 1.9363752 | 1.6411 | 3.5 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_110669_M1Hsky_S08
111064 | 149.6323822 | 1.9393212 | 1.6164 | 3.5 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_111064_M1Hsky_S15
115146 | 149.6558387 | 1.9476929 | 2.5189 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_115146_M1Ksky_S14
116202 | 149.6839698 | 1.9502112 | 1.5329 | 3.5 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_116202_M1Hsky_S13
121050 | 149.6511528 | 1.961198 | 1.5708 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_121050_M1Hsky_S16
121736 | 149.6605124 | 1.9621859 | 2.1603 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_121736_M1Ksky_S17
193269 | 149.9183382 | 2.1055916 | 1.3605 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_193269_M25Hsky_S15
194648 | 149.7419169 | 2.1075764 | 1.5313 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_194648_M3Hsky_S10
197419 | 149.9092285 | 2.1130251 | 1.4708 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_197419_M25Hsky_S08
199380 | 149.9150387 | 2.1170209 | 2.2631 | 4.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_199380_M25Ksky_S09
201260 | 149.8729828 | 2.1204449 | 2.3737 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_201260_M25Ksky_S08
202778 | 149.8772597 | 2.1237659 | 1.5083 | 3.5 |  H$\alpha$ | COSMOS_LBT_APR21_1d_202778_M25Hsky_S17
209194 | 149.7100321 | 2.136129 | 2.3874 | 3.0 |  [O iii] | COSMOS_LBT_MAR20_1d_209194_M3Hsky_S22
209927 | 149.9253192 | 2.134973 | 1.6063 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_209927_M25Hsky_S22
210275 | 150.4068985 | 2.1383306 | 1.6417 | 3.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_210275_M12Hsky_S11
211581 | 149.7091359 | 2.1392878 | 1.6414 | 3.5 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_211581_M3Hsky_S14
211984 | 149.8673655 | 2.1410346 | 2.4487 | 4.0 |  [O iii] | COSMOS_LBT_APR21_1d_211984_M25Hsky_S18
215091 | 149.9281427 | 2.1470197 | 2.3757 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_215091_M25Ksky_S21
217459 | 149.7618337 | 2.1518038 | 1.6168 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_217459_M3Hsky_S08
218192 | 149.904775 | 2.15362 | 2.3852 | 4.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_218192_M25Ksky_S11
218228 | 149.717966 | 2.1530929 | 2.4342 | 3.5 |  [O iii] | COSMOS_LBT_MAR20_1d_218228_M3Hsky_S21
218763 | 149.7468821 | 2.1537101 | 1.6377 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_218763_M3Hsky_S17
219390 | 149.7583034 | 2.1559746 | 1.5267 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_219390_M3Hsky_S18
220827 | 150.4434614 | 2.1586643 | 1.5392 | 4.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_220827_M12Hsky_S10
221149 | 150.4139644 | 2.1591002 | 1.5572 | 4.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_221149_M12Hsky_S09
223074 | 149.8970859 | 2.1622611 | 2.2388 | 3.0 |  [O iii] | COSMOS_LBT_MAR21_1d_223074_M25Hsky_S20
224872 | 149.8749001 | 2.1660171 | 1.5268 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_224872_M25Hsky_S12
226236 | 149.7460689 | 2.1675662 | 2.4344 | 4.0 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_226236_M3Ksky_S17
226249 | 150.4191533 | 2.1687531 | 1.5962 | 3.5 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_226249_M12Hsky_S19
234751 | 150.4445932 | 2.1847414 | 1.5192 | 3.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_234751_M12Hsky_S13
248229 | 150.1880526 | 2.2102579 | 2.4808 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR21_1d_248229_LAE4Ksky_S13
251341 | 149.7751888 | 2.216971 | 2.3177 | 4.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_251341_M29Ksky_S12
251539 | 149.825632 | 2.217383 | 2.4540 | 4.0 |  [O iii] | COSMOS_LBT_APR21_1d_251539_M29Hsky_S20
253054 | 149.7693121 | 2.2208096 | 1.4158 | 4.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_253054_M29Hsky_S14
254879 | 150.0895379 | 2.2235747 | 1.3521 | 3.0 |  H$\alpha$ | COSMOS_LBT_MAR20_1d_254879_M2Hsky_S17
256237 | 149.8125082 | 2.2260419 | 1.5503 | 4.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_256237_M29Hsky_S16
261029 | 149.8140962 | 2.234968 | 1.6858 | 3.5 |  H$\alpha$ | COSMOS_LBT_APR21_1d_261029_M29Hsky_S17
261242 | 150.1912935 | 2.2358824 | 2.2798 | 4.0 |  H$\alpha$ | COSMOS_LBT_MAR21_1d_261242_LAE4Ksky_S21
263941 | 149.802669 | 2.2413337 | 2.2147 | 3.5 |  H$\alpha$ | COSMOS_LBT_APR21_1d_263941_M29Ksky_S08
272390 | 150.4427008 | 2.2577357 | 1.5845 | 4.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_272390_M24Hsky_S15
277689 | 150.4825951 | 2.2692277 | 1.5850 | 4.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_277689_M24Hsky_S10
281625 | 150.489104 | 2.2775923 | 1.6303 | 4.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_281625_M24Hsky_S11
305682 | 149.9338397 | 2.325281 | 1.6150 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_305682_M22Hsky_S14
Table 1: continued.  OBJ_ID | RA | Dec | $z_{\rm spec}$ | Flag | Line | 1D-Spectum
---|---|---|---|---|---|---
311645 | 149.7982448 | 2.3368401 | 1.6048 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_311645_M27Hsky_S15
315750 | 150.3914582 | 2.3435241 | 1.4790 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_315750_M14Hsky_S09
320989 | 149.8092325 | 2.3544984 | 2.3707 | 3.0 |  [O iii] | COSMOS_LBT_APR21_1d_320989_M27Hsky_S21
321846 | 150.3609407 | 2.3563503 | 1.5855 | 3.5 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_321846_M18Hsky_S21
323850 | 149.9217085 | 2.3597902 | 2.1015 | 4.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_323850_M22Ksky_S09
326545 | 150.3990555 | 2.3652568 | 1.4830 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_326545_M14Hsky_S08
328061 | 150.3336896 | 2.3676283 | 1.6350 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_328061_M18Hsky_S14
329209 | 150.338739 | 2.3703542 | 1.5800 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_329209_M18Hsky_S09
330051 | 149.8129738 | 2.3717757 | 1.6053 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_330051_M27Hsky_S08
331551 | 149.804426 | 2.3743435 | 1.6261 | 3.5 |  H$\alpha$ | COSMOS_LBT_APR21_1d_331551_M27Hsky_S17
331974 | 149.791189 | 2.3754079 | 1.4323 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_331974_M27Hsky_S10
332036 | 149.7654438 | 2.3750567 | 1.5273 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_332036_M27Hsky_S13
334638 | 150.3069896 | 2.3796186 | 1.5800 | 4.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_334638_M17Hsky_S19
336706 | 150.3182657 | 2.383641 | 1.3850 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_336706_M17Hsky_S09
340178 | 150.3197125 | 2.3908843 | 2.5510 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_340178_M17Ksky_S11
344560 | 150.3518992 | 2.4002879 | 1.4320 | 4.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_344560_M18Hsky_S18
346399 | 150.2869306 | 2.4032503 | 1.4390 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_346399_M17Hsky_S14
347369 | 150.2775421 | 2.4062789 | 1.5020 | 4.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_347369_M17Hsky_S10
348742 | 150.3284294 | 2.4085777 | 1.4830 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_348742_M17Hsky_S08
349330 | 150.3218736 | 2.4103132 | 2.4720 | 3.5 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_349330_M17Ksky_S08
385760 | 149.8700627 | 2.4886839 | 1.5598 | 3.5 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_385760_M10Hsky_S18
400371 | 149.8867628 | 2.5176858 | 1.5830 | 3.5 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_400371_M9Hsky_S14
402003 | 149.8499016 | 2.5216286 | 1.6036 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_402003_M10Hsky_S24
402635 | 149.8462499 | 2.5224695 | 2.1713 | 3.0 |  [O iii] | COSMOS_LBT_DEC20_1d_402635_M10Hsky_S19
402635 | 149.8462499 | 2.5224695 | 2.1703 | 4.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_402635_M10Ksky_S12
404898 | 149.9153074 | 2.5273345 | 2.2453 | 3.5 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_404898_M9Ksky_S10
406056 | 149.9333663 | 2.5297759 | 2.4252 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_406056_M9Ksky_S12
406594 | 149.8966304 | 2.5305503 | 2.2363 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_406594_M9Ksky_S15
407529 | 149.8794106 | 2.5322392 | 1.5838 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_407529_M10Hsky_S20
409697 | 149.9326151 | 2.5364134 | 2.2453 | 4.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_409697_M9Ksky_S13
412341 | 149.8873947 | 2.5422249 | 2.2493 | 4.0 |  [O iii] | COSMOS_LBT_DEC20_1d_412341_M10Hsky_S21
417124 | 149.9357984 | 2.5514111 | 2.1963 | 3.0 |  [O iii] | COSMOS_LBT_DEC20_1d_417124_M9Hsky_S19
421534 | 149.919234 | 2.5604157 | 2.3243 | 4.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_421534_M9Ksky_S14
423163 | 149.9075378 | 2.5636165 | 1.5572 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_423163_M9Hsky_S22
426464 | 149.8888229 | 2.569995 | 1.6652 | 3.5 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_426464_M9Hsky_S17
427350 | 149.9084958 | 2.5712201 | 1.6607 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_427350_M9Hsky_S13
459855 | 150.0530532 | 2.6369884 | 1.4466 | 3.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_459855_M7Hsky_S10
462025 | 150.0826055 | 2.6413449 | 2.0873 | 3.0 |  [O iii] | COSMOS_LBT_DEC20_1d_462025_M7Hsky_S15
462025 | 150.0826055 | 2.6413449 | 2.0877 | 3.0 |  [O iii] | COSMOS_LBT_JAN21_1d_462025_M7Hsky_S15
463893 | 150.4854222 | 2.6455409 | 2.3473 | 4.0 |  [O iii] | COSMOS_LBT_DEC20_1d_463893_M6Hsky_S24
463893 | 150.4854222 | 2.6455409 | 2.3473 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_463893_M6Ksky_S14
465574 | 150.4536772 | 2.6487302 | 2.4120 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_465574_M15Ksky_S15
468350 | 150.48936 | 2.6544405 | 2.3955 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_468350_M6Ksky_S13
472716 | 150.2653786 | 2.6627636 | 1.7120 | 3.5 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_472716_M8Hsky_S16
472716 | 150.2653786 | 2.6627636 | 1.7122 | 3.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_472716_M8Hsky_S16
474523 | 150.0922862 | 2.6656468 | 2.2117 | 3.5 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_474523_M7Ksky_S09
475417 | 150.0911944 | 2.6683391 | 2.5042 | 3.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_475417_M7Ksky_S18
475527 | 150.0591837 | 2.6685413 | 2.4372 | 4.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_475527_M7Ksky_S11
476044 | 149.9910794 | 2.6692601 | 1.5645 | 4.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_476044_M11Hsky_S15
476459 | 150.4419312 | 2.6701195 | 1.6134 | 3.5 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_476459_M15Hsky_S20
476771 | 150.5134492 | 2.66873 | 1.5792 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_476771_M6Hsky_S21
478878 | 150.4690208 | 2.675255 | 1.6122 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_478878_M6Hsky_S25
479007 | 150.0857052 | 2.6747758 | 2.2723 | 4.0 |  [O iii] | COSMOS_LBT_DEC20_1d_479007_M7Hsky_S16
479007 | 150.0857052 | 2.6747758 | 2.2722 | 4.0 |  [O iii] | COSMOS_LBT_JAN21_1d_479007_M7Hsky_S16
479007 | 150.0857052 | 2.6747758 | 2.2730 | 4.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_479007_M7Ksky_S08
480046 | 150.056362 | 2.6768332 | 2.2702 | 4.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_480046_M7Ksky_S15
480239 | 150.2307456 | 2.6769689 | 1.5994 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_480239_M8Hsky_S09
480640 | 150.5207857 | 2.6781376 | 1.5732 | 3.5 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_480640_M6Hsky_S13
481315 | 150.2668853 | 2.67968 | 2.4913 | 4.0 |  [O iii] | COSMOS_LBT_DEC20_1d_481315_M8Hsky_S19
481315 | 150.2668853 | 2.67968 | 2.4907 | 4.0 |  [O iii] | COSMOS_LBT_JAN21_1d_481315_M8Hsky_S19
481317 | 150.4749598 | 2.6794807 | 1.5390 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_481317_M15Hsky_S12
481647 | 150.2672757 | 2.6799633 | 1.5010 | 4.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_481647_M8Hsky_S19
481647 | 150.2672757 | 2.6799633 | 1.5010 | 4.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_481647_M8Hsky_S19
482104 | 150.4218192 | 2.681305 | 2.1450 | 3.0 |  [O iii] | COSMOS_LBT_FEB21_1d_482104_M15Hsky_S18
483394 | 150.5219636 | 2.6838403 | 2.2158 | 4.0 |  [O iii] | COSMOS_LBT_DEC20_1d_483394_M6Hsky_S20
483647 | 150.2127732 | 2.6836628 | 2.2242 | 3.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_483647_M8Ksky_S17
484275 | 149.9975234 | 2.6859328 | 2.0482 | 3.0 |  [O iii] | COSMOS_LBT_JAN21_1d_484275_M11Hsky_S19
484310 | 150.2587791 | 2.6852644 | 1.5882 | 3.5 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_484310_M8Hsky_S22
484310 | 150.2587791 | 2.6852644 | 1.5876 | 3.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_484310_M8Hsky_S22
484662 | 150.0656512 | 2.6864807 | 1.4061 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_484662_M7Hsky_S11
486496 | 150.5087376 | 2.7042991 | 1.5354 | 3.5 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_486496_M6Hsky_S15
486866 | 149.967041 | 2.6964446 | 1.4401 | 3.5 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_486866_M11Hsky_S14
489100 | 150.4748461 | 2.6867608 | 1.6377 | 4.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_489100_M6Hsky_S17
489314 | 149.9812037 | 2.6941987 | 2.2162 | 3.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_489314_M11Ksky_S19
490030 | 149.9783643 | 2.7028003 | 2.3922 | 4.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_490030_M11Ksky_S12
492453 | 150.2442763 | 2.7067051 | 2.4702 | 3.0 |  H$\alpha$ | COSMOS_LBT_JAN21_1d_492453_M8Ksky_S20
Table 1: continued.  OBJ_ID | RA | Dec | $z_{\rm spec}$ | Flag | Line | 1D-Spectum
---|---|---|---|---|---|---
494350 | 150.4846551 | 2.6939799 | 1.6412 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_494350_M6Hsky_S14
549854 | 149.907150209 | 2.137621434 | 1.4802 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_549854_M25Hsky_S10
603116 | 150.197082912 | 2.21687046 | 2.4638 | 4.0 |  H$\alpha$ | COSMOS_LBT_MAR21_1d_603116_LAE4Ksky_S19
621780 | 150.471209414 | 2.2446394 | 2.4847 | 4.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_621780_M24Ksky_S08
646613 | 150.468731703 | 2.281641135 | 1.4908 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_646613_M24Hsky_S12
703468 | 149.78839164 | 2.36554692 | 2.3277 | 3.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_703468_M27Ksky_S09
720513 | 149.803548302 | 2.391162136 | 2.2512 | 4.0 |  H$\alpha$ | COSMOS_LBT_APR21_1d_720513_M27Ksky_S13
732820 | 150.302551814 | 2.411721348 | 1.6495 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_732820_M17Hsky_S13
811438 | 149.876631272 | 2.530976324 | 2.3623 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_811438_M9Ksky_S18
811438 | 149.876631272 | 2.530976324 | 2.3618 | 3.0 |  H$\alpha$ | COSMOS_LBT_DEC20_1d_811438_M10Ksky_S15
911024 | 150.434047436 | 2.68423913 | 2.2965 | 3.0 |  H$\alpha$ | COSMOS_LBT_FEB21_1d_911024_M15Ksky_S18
914020 | 150.445804162 | 2.685678498 | 1.5730 | 3.0 | Pa | COSMOS_LBT_FEB21_1d_914020_M15Ksky_S24
3324 | 36.6244607 | $-4.9884302$ | 1.5340 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_3324_M3Hsky_S16
3324 | 36.6244607 | $-4.9884302$ | 1.5339 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_3324_M3Hsky_S16
6892 | 36.5680458 | $-4.9803015$ | 2.2071 | 3.0 |  [O iii] | VVDS_LBT_OCT19_1d_6892_M3Hsky_S21
7941 | 36.6288502 | $-4.9780309$ | 1.5346 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_7941_M3Hsky_S17
7941 | 36.6288502 | $-4.9780309$ | 1.5346 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT19_1d_7941_M3Hsky_S17
15031 | 36.509626 | $-4.9637322$ | 2.0701 | 3.0 |  [O iii] | VVDS_LBT_OCT20_1d_15031_M4Hsky_S23
19965 | 36.5629042 | $-4.9542579$ | 1.5200 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT19_1d_19965_M1Hsky_S17
21178 | 36.5418393 | $-4.9519901$ | 1.5304 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_21178_M1Hsky_S16
21370 | 36.5334932 | $-4.9518214$ | 2.3841 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_21370_M4Ksky_S13
22805 | 36.528381 | $-4.9487815$ | 1.5334 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_22805_M4Hsky_S16
22805 | 36.528381 | $-4.9487815$ | 1.5331 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT19_1d_22805_M4Hsky_S16
24882 | 36.5648159 | $-4.94453$ | 1.3761 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_24882_M3Hsky_S11
24882 | 36.5648159 | $-4.94453$ | 1.3761 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_24882_M1Hsky_S18
24882 | 36.5648159 | $-4.94453$ | 1.3766 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_24882_M3Hsky_S11
24903 | 36.5064947 | $-4.9450216$ | 1.5781 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_24903_M4Hsky_S21
24903 | 36.5064947 | $-4.9450216$ | 1.5781 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_24903_M4Hsky_S21
29861 | 36.59385 | $-4.9345849$ | 2.0941 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_29861_M3Ksky_S20
30293 | 36.582892 | $-4.9341326$ | 1.5335 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_30293_M1Hsky_S11
34978 | 36.6069178 | $-4.9249799$ | 1.5624 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_34978_M2Hsky_S16
36412 | 36.587422 | $-4.922475$ | 1.5366 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_36412_M1Hsky_S20
36412 | 36.587422 | $-4.922475$ | 1.5366 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_36412_M2Hsky_S15
37921 | 36.493333 | $-4.9206908$ | 2.0007 | 3.0 |  [O iii] | VVDS_LBT_OCT20_1d_37921_M4Hsky_S24
37921 | 36.493333 | $-4.9206908$ | 2.0006 | 4.0 |  [O iii] | VVDS_LBT_OCT19_1d_37921_M4Hsky_S24
38524 | 36.6009144 | $-4.9185782$ | 1.5464 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_38524_M2Hsky_S13
39192 | 36.5348629 | $-4.9172989$ | 2.0604 | 4.0 |  [O iii] | VVDS_LBT_OCT19_1d_39192_M1Hsky_S22
40659 | 36.4435417 | $-4.9146046$ | 1.6057 | 4.0 |  H$\alpha$ | VVDS_LBT_JAN20_1d_40659_M9Hsky_S14
44310 | 36.5107537 | $-4.9075348$ | 1.3711 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT19_1d_44310_M4Hsky_S12
45642 | 36.517377 | $-4.9061548$ | 2.0616 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_45642_M4Ksky_S20
47083 | 36.4888123 | $-4.9021975$ | 1.6245 | 4.0 |  H$\alpha$ | VVDS_LBT_JAN20_1d_47083_M9Hsky_S17
49143 | 36.4810046 | $-4.8989504$ | 2.4147 | 4.0 |  [O iii] | VVDS_LBT_JAN20_1d_49143_M9Hsky_S11
50696 | 36.5757347 | $-4.8950953$ | 1.5200 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT19_1d_50696_M2Hsky_S17
51100 | 36.4519719 | $-4.8943098$ | 1.5836 | 3.0 |  H$\alpha$ | VVDS_LBT_JAN20_1d_51100_M9Hsky_S12
52018 | 36.6037449 | $-4.8923901$ | 1.6183 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT19_1d_52018_M2Hsky_S18
54789 | 36.8943492 | $-4.8870347$ | 1.4426 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_54789_M6Hsky_S14
55141 | 36.4425414 | $-4.8865782$ | 2.2326 | 3.0 |  H$\alpha$ | VVDS_LBT_JAN20_1d_55141_M9Ksky_S17
56255 | 36.6051263 | $-4.8844258$ | 1.5303 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_56255_M2Hsky_S12
56891 | 36.5720134 | $-4.884359$ | 2.2711 | 3.0 |  [O iii] | VVDS_LBT_OCT19_1d_56891_M2Hsky_S19
57263 | 36.8684341 | $-4.882315$ | 2.2801 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_57263_M6Ksky_S11
64030 | 36.8392892 | $-4.8692322$ | 2.3328 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_64030_M6Ksky_S17
66084 | 36.8538979 | $-4.8654714$ | 2.2856 | 4.0 |  [O iii] | VVDS_LBT_OCT20_1d_66084_M6Hsky_S21
68382 | 36.8625965 | $-4.863006$ | 1.5341 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_68382_M6Hsky_S17
68592 | 36.4582577 | $-4.8616541$ | 1.5203 | 3.0 |  H$\alpha$ | VVDS_LBT_JAN20_1d_68592_M9Hsky_S18
68635 | 36.4673469 | $-4.8614609$ | 2.2052 | 4.0 |  [O iii] | VVDS_LBT_JAN20_1d_68635_M9Hsky_S24
77168 | 36.8614225 | $-4.8455261$ | 1.5259 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_77168_M6Hsky_S13
125460 | 36.118401 | $-4.7518593$ | 1.4856 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_125460_M13Hsky_S16
125920 | 36.1522153 | $-4.7512865$ | 1.7006 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_125920_M13Hsky_S15
127119 | 36.1466843 | $-4.7480526$ | 2.1141 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_127119_M13Ksky_S16
128166 | 36.1172243 | $-4.7457655$ | 2.0408 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_128166_M13Ksky_S11
135766 | 36.0902942 | $-4.7310129$ | 2.2975 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_135766_M13Ksky_S14
137799 | 36.1486107 | $-4.7260611$ | 2.2142 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_137799_M13Ksky_S15
138587 | 36.1042005 | $-4.7247136$ | 1.6776 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_138587_M13Hsky_S12
138945 | 36.5706378 | $-4.7236601$ | 2.2062 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_138945_M5Ksky_S17
140031 | 36.0898178 | $-4.7212704$ | 2.2141 | 4.0 |  [O iii] | VVDS_LBT_OCT20_1d_140031_M13Hsky_S19
140031 | 36.0898178 | $-4.7212704$ | 2.2141 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_140031_M13Ksky_S18
140527 | 36.635215 | $-4.7209197$ | 2.1296 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_140527_M5Ksky_S21
142226 | 36.6331479 | $-4.7173309$ | 1.5164 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_142226_M5Hsky_S15
142226 | 36.6331479 | $-4.7173309$ | 1.5166 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_142226_M5Hsky_S15
144923 | 36.2271709 | $-4.7120479$ | 1.5601 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_144923_M5Hsky_S14
144923 | 36.2271709 | $-4.7120479$ | 1.5600 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_144923_M5Hsky_S14
147228 | 36.1020614 | $-4.7087143$ | 1.5386 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_147228_M13Hsky_S13
154912 | 36.34384 | $-4.6933544$ | 2.1396 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_154912_M11Ksky_S14
158984 | 36.3422744 | $-4.6854868$ | 2.1911 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_158984_M11Ksky_S12
Table 1: continued.  OBJ_ID | RA | Dec | $z_{\rm spec}$ | Flag | Line | 1D-Spectum
---|---|---|---|---|---|---
160224 | 36.6517582 | $-4.6828961$ | 1.6061 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_160224_M5Hsky_S11
160224 | 36.6517582 | $-4.6828961$ | 1.6061 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_160224_M14Hsky_S12
160224 | 36.6517582 | $-4.6828961$ | 1.6061 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_160224_M5Hsky_S11
162982 | 36.6420709 | $-4.6787762$ | 2.2448 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_162982_M5Ksky_S12
162982 | 36.6420709 | $-4.6787762$ | 2.2435 | 4.0 |  [O iii] | VVDS_LBT_OCT19_1d_162982_M5Hsky_S20
163515 | 36.6101764 | $-4.6765857$ | 1.5716 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_163515_M5Hsky_S16
163515 | 36.6101764 | $-4.6765857$ | 1.5716 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_163515_M14Hsky_S15
163515 | 36.6101764 | $-4.6765857$ | 1.5717 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT19_1d_163515_M5Hsky_S16
165659 | 36.3549882 | $-4.6723701$ | 2.1395 | 3.0 |  [O iii] | VVDS_LBT_OCT20_1d_165659_M11Hsky_S19
165659 | 36.3549882 | $-4.6723701$ | 2.1396 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_165659_M11Ksky_S11
165940 | 36.6296705 | $-4.671717$ | 2.2646 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_165940_M5Ksky_S20
165940 | 36.6296705 | $-4.671717$ | 2.2651 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_165940_M14Ksky_S19
166946 | 36.3469914 | $-4.669578$ | 2.2211 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_166946_M11Ksky_S15
167263 | 36.6519619 | $-4.6694611$ | 2.2601 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_167263_M5Ksky_S13
167263 | 36.6519619 | $-4.6694611$ | 2.2596 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_167263_M14Ksky_S13
167264 | 36.6445147 | $-4.6690833$ | 2.2581 | 3.0 |  [O iii] | VVDS_LBT_OCT20_1d_167264_M5Hsky_S19
167264 | 36.6445147 | $-4.6690833$ | 2.2601 | 3.0 |  [O iii] | VVDS_LBT_OCT19_1d_167264_M5Hsky_S19
168107 | 36.650895 | $-4.668188$ | 1.5596 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_168107_M5Hsky_S13
168107 | 36.650895 | $-4.668188$ | 1.5601 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT19_1d_168107_M5Hsky_S13
168869 | 36.6114714 | $-4.6661429$ | 2.4436 | 4.0 |  [O iii] | VVDS_LBT_OCT20_1d_168869_M14Hsky_S21
168869 | 36.6114714 | $-4.6661429$ | 2.4429 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_168869_M14Ksky_S15
170223 | 36.3308287 | $-4.6636302$ | 2.2088 | 3.0 |  [O iii] | VVDS_LBT_OCT20_1d_170223_M11Hsky_S17
171656 | 36.638702 | $-4.6610195$ | 2.2376 | 3.0 |  [O iii] | VVDS_LBT_OCT20_1d_171656_M14Hsky_S19
171656 | 36.638702 | $-4.6610195$ | 2.2375 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_171656_M14Ksky_S21
171798 | 36.6554476 | $-4.6607726$ | 2.2481 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_171798_M14Ksky_S20
172082 | 36.6448409 | $-4.660273$ | 1.5301 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_172082_M8Hsky_S16
172693 | 36.6565846 | $-4.659415$ | 1.4361 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_172693_M8Hsky_S13
174768 | 36.6440171 | $-4.654438$ | 1.6161 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_174768_M14Hsky_S13
176272 | 36.319106 | $-4.6532566$ | 1.5617 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_176272_M11Hsky_S14
178570 | 36.6703436 | $-4.6478391$ | 1.4899 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_178570_M8Hsky_S11
178934 | 36.3514434 | $-4.6468935$ | 1.5924 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_178934_M11Hsky_S15
179071 | 36.3389785 | $-4.6466188$ | 2.1121 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_179071_M11Ksky_S18
179905 | 36.6104572 | $-4.6444695$ | 2.0608 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_179905_M8Ksky_S17
179905 | 36.6104572 | $-4.6444695$ | 2.0601 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_179905_M14Ksky_S11
179990 | 36.6410461 | $-4.6449848$ | 2.0356 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_179990_M8Ksky_S15
179990 | 36.6410461 | $-4.6449848$ | 2.0356 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_179990_M14Ksky_S14
180446 | 36.3482592 | $-4.6438773$ | 1.5936 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_180446_M11Hsky_S13
181261 | 36.6620577 | $-4.6416814$ | 2.1613 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_181261_M8Ksky_S12
182940 | 36.6496611 | $-4.6387972$ | 1.4648 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_182940_M8Hsky_S12
185040 | 36.6119311 | $-4.6349522$ | 2.2231 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_185040_M8Ksky_S16
185523 | 36.6239302 | $-4.6337579$ | 2.0396 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_185523_M14Ksky_S12
364094 | 36.1562797 | $-4.3005582$ | 1.6041 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_364094_M12Hsky_S12
365897 | 36.1601525 | $-4.2975043$ | 2.2641 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_365897_M12Ksky_S13
369449 | 36.1630987 | $-4.2916442$ | 2.1381 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_369449_M12Ksky_S12
370077 | 36.1404797 | $-4.2901132$ | 2.2831 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_370077_M12Ksky_S14
373735 | 36.1359352 | $-4.2834295$ | 2.3121 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_373735_M12Ksky_S20
383107 | 36.1552194 | $-4.265314$ | 2.1861 | 3.0 |  [O iii] | VVDS_LBT_OCT20_1d_383107_M12Hsky_S19
383107 | 36.1552194 | $-4.265314$ | 2.1861 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_383107_M12Ksky_S19
384395 | 36.1729741 | $-4.2637323$ | 1.5656 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_384395_M12Hsky_S16
385771 | 36.1347704 | $-4.25996$ | 1.5660 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_385771_M12Hsky_S15
390991 | 36.134847 | $-4.2505199$ | 1.7036 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_390991_M12Hsky_S14
395770 | 36.1589829 | $-4.2421372$ | 2.0961 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_395770_M12Ksky_S16
433842 | 36.3966135 | $-4.1783018$ | 2.1341 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_433842_M10Ksky_S18
434177 | 36.378452 | $-4.1779649$ | 1.6138 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_434177_M10Hsky_S11
437678 | 36.4035061 | $-4.1727462$ | 2.2566 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_437678_M10Ksky_S17
439294 | 36.3874695 | $-4.1691679$ | 1.6311 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_439294_M10Hsky_S12
444135 | 36.3733867 | $-4.1615026$ | 2.1692 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_444135_M10Ksky_S16
446244 | 36.4085951 | $-4.1577974$ | 1.5561 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_446244_M10Hsky_S13
447002 | 36.4085929 | $-4.1569321$ | 1.5541 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_447002_M10Hsky_S13
511951 | 36.2024782 | $-4.0510283$ | 1.4936 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_511951_M7Hsky_S14
513770 | 36.1631932 | $-4.0473276$ | 2.1621 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_513770_M7Ksky_S15
515718 | 36.1910121 | $-4.043192$ | 2.3256 | 3.0 |  [O iii] | VVDS_LBT_OCT20_1d_515718_M7Hsky_S23
515718 | 36.1910121 | $-4.043192$ | 2.3261 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_515718_M7Ksky_S16
523367 | 36.2055719 | $-4.0311235$ | 1.6041 | 3.5 |  H$\alpha$ | VVDS_LBT_OCT20_1d_523367_M7Hsky_S15
527425 | 36.1997576 | $-4.0239239$ | 2.2281 | 3.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_527425_M7Ksky_S13
540741 | 36.1744902 | $-4.0002201$ | 2.2516 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_540741_M7Ksky_S23
542094 | 36.1703008 | $-4.0064452$ | 1.6061 | 4.0 |  H$\alpha$ | VVDS_LBT_OCT20_1d_542094_M7Hsky_S11