# WALLABY Pilot Survey: the Tully-Fisher relation in the NGC 4808, Vela and
NGC 5044 fields

Jeremy Mould,1,2 T. H. Jarrett,3 Hélène Courtois4 Albert Bosma5 Nathan Deg14
Alexandra Dupuy8 Lister Staveley-Smith9,10 E.N. Taylor1 Jayanne English20 S.
H. A. Rajohnson21 Renée Kraan-Korteweg21 Duncan Forbes1 Helga Dénes7 Karen
Lee-Waddell6,9,10 Austin Shen18,19 O. I. Wong6,9,16 Benne Holwerda13 Bärbel
Koribalski11,12 Denis Leahy22 Pavel Mancera Piña15 Niankun Yu17,23

1Centre for Astrophysics & Supercomputing, Swinburne University, Hawthorn, VIC
3122, Australia.
2ARC Centre of Excellence for Dark Matter Particle Physics
3Astronomy Department, University of Cape Town, Private Bag X3, Rondebosch
7701, South Africa
4UCB Lyon 1, IUF IP21, Lyon, 69622, Villeurbanne, France.
5Aix Marseille University, CNRS, CNES, LAM Marseille, France.
6CSIRO Space & Astronomy, PO Box 1130, Bentley, WA 6102, Australia.
7School of Physical Science & Nanotechnology, Yachay Tech University, Hacienda
San José S/N 100119, Urcuquí, Ecuador.
8Korea Institute for Advanced Study, 85, Hoegi-ro, Dongdaemun-gu, Seoul 02455,
Republic of Korea.
9ICRAR-M468, University of Western Australia, 35 Stirling Highway, Crawley, WA
6009, Australia.
10ICRAR - Curtin University, Bentley. WA 6102, Australia.
11Australia Telescope National Facility, CSIRO Astronomy & Space Science, PO
Box 76, Epping, NSW 1710, Australia.
12School of Science, Western Sydney University, Locked Bag 1797, Penrith, NSW
2751, Australia.
13University of Louisville, Department of Physics & Astronomy, Louisville KY
40292, USA.
14Department of Physics, Engineering Physics & Astronomy, Queen’s University,
Kingston, ON, K7L 3N6, Canada.
15Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, The
Netherlands
16ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO
3D).
17National Astronomical Observatories, Chinese Academy of Sciences, Beijing,
100101, P.R. China
18CSIRO Space & Astronomy, PO Box 1130, Bentley, WA 6102, Australia
19Australian SKA Regional Centre (AusSRC)
20Department of Physics and Astronomy, University of Manitoba, Winnipeg,
Manitoba, Canada, R3T 2N2, Canada
21Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch
7701, South Africa
22Department of Physics and Astronomy, University of Calgary, Calgary, AB T2N
1N4, Canada
23Key Laboratory of Radio Astronomy and Technology, Chinese Academy of
Sciences, Beijing, 100101, P.R. China E-mail<EMAIL_ADDRESS>
(Accepted 2024 June 14. Received 2024 June 13; in original form 2024 May 8)

###### Abstract

The Tully-Fisher Relation (TFR) is a well-known empirical relationship between
the luminosity of a spiral galaxy and its circular velocity, allowing us to
estimate redshift independent distances. Here we use high signal-to-noise HI
21-cm integrated spectra from the second pilot data release (PDR2, 180 deg2)
of the Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY). In order
to prepare for the full WALLABY survey, we have investigated the TFR in phase
2 of the pilot survey with a further three fields. The data were obtained with
wide-field Phased Array Feeds on the Australian Square Kilometre Array
Pathfinder (ASKAP) and have an angular resolution of 30 arcsec and a velocity
resolution of $\sim$4 km s-1. Galaxy luminosities have been measured from the
Wide-field Infrared Survey Explorer (WISE), and optical galaxy inclinations
from the Dark Energy Camera Legacy Survey. We present TFRs for wavelengths
from 0.8–3.4$\mu$m. We examine sources of galaxy inclination data and
investigate magnitudes from the DECam Local Volume Exploration Survey (DELVE)
and DENIS catalogues and the 4HS target catalogue based on the VISTA
Hemisphere Survey (VHS). We consider the baryonic TFR. These are all of
interest for TFR using the full WALLABY survey of 200,000 galaxies. We
demonstrate that WALLABY TFR distances can take their place among state of the
art studies of the local velocity field.

###### keywords:

large scale structure of the Universe, surveys, infrared photometry, radio
astronomy

††pubyear: 2024††pagerange: WALLABY Pilot Survey: the Tully-Fisher relation in
the NGC 4808, Vela and NGC 5044 fields–A0.4

##  1 Introduction

In the local Universe large-scale structure can be investigated using
redshift- independent distance indicators, such as the Tully-Fisher Relation
(TFR), which allow galaxies’ peculiar velocities to be measured. Peculiar
velocities come about because mass density inhomogeneities in the Universe act
on galaxies and perturb the velocities given to them by the expansion of the
Universe. To be exact, the peculiar velocity of a galaxy arises from the
volume integral of the overdensities divided by the square of the distances to
them, multiplied by the growth rate. Here the over-density is $\delta$ =
$\delta\rho/\bar{\rho}-1$ where $\rho$ and $\bar{\rho}$ are the density and
mean density of the Universe, and the growth rate, $f$, is approximately
$\Omega_{m}^{4/7}$ in the $\Lambda$CDM standard model, where $\Omega_{m}$ is
the mass density parameter. Peculiar velocities have therefore been used to
constrain the cosmological parameter $f\sigma_{8}$ ($\sigma_{8}$ is the
amplitude of the power spectrum on scales of 8$h^{-1}$ Mpc; Adams & Blake
2017; Dupuy et al. 2019), thus providing a test of gravity on very large
scales. To measure peculiar velocities we need redshift-independent distance
indicators, such as the Fundamental Plane (Djorgovski & Davis 1987),the
supernova standard candle (Kowal 1968) and the Tully-Fisher relation (Tully &
Fisher 1977).

Figure 1: WALLABY galaxies in the NGC4808 field in the supergalactic plane.
The long axis is the heliocentric recession velocity in the SGY direction, and
the vertical axis is the the heliocentric recession velocity in the SGX
direction.The structure is evident in galaxy groups and filaments.

The Widefield ASKAP L-band Legacy All-sky Blind surveY (or WALLABY; Koribalski
et al. 2020) is being conducted on the Australian SKA Pathfinder (ASKAP, Hotan
et al. 2021), an innovative imaging radio telescope located at the Murchison
Radio-astronomy Observatory in Western Australia. The aim of WALLABY is to use
the powerful widefield phased-array technology of ASKAP to observe initially
14,000 square degrees of the southern hemisphere in the 21-cm line of neutral
hydrogen at 30-arcsec resolution (Westmeier et al. 2022)111Sky coverage is
described at https://wallaby-survey.org/overview/. The survey began in January
2023, but a number of fields were observed in 2022 as a pilot program, among
them the phase 2 target fields centred on NGC 4808, Vela and NGC 5044. WALLABY
pilot survey phase 2 data were released in DR2 by Murugeshan et al. (2024).

The goals of this paper are first to learn as much as possible about the
Tully-Fisher Relation (TFR) early on, since the full WALLABY Survey will be a
hundred times larger than the pilot survey, and, second, to measure peculiar
velocities to be compared with expectations from the CosmicFlows program
(Courtois & Tully 2015).

In the paper we extract and measure HI spectra of galaxies in these fields and
combine them ($\S\S$2,3 & 4) with customized WISE total magnitudes (Jarrett et
al. 2023). Infrared photometry has the advantage of being less affected by
extinction in our Galaxy and the target galaxies (Aaronson, Huchra & Mould
1979). We also investigate available I band photometry and optical diameters.
The utility of WALLABY for peculiar velocity measurement is considered in
$\S$5, and our conclusions are summarized in $\S$6.

##  2 The NGC 4808 field

Source finding using SoFiA (Westmeier et al. 2021; Serra et al. 2015) and HI
measurements for the NGC 4808 field follow Courtois et al. (2022; Paper 1).
SoFiA2 uses the Smooth + Clip algorithm for source finding, which operates by
spatially and spectrally smoothing the data on multiple scales and applying a
user-defined flux threshold relative to the noise level in each iteration. A
wide range of useful preconditioning and post-processing filters is available,
including noise normalization, flagging of artifacts and reliability
filtering. Values of W50 were measured directly from the flux density versus
frequency spectra produced by the WALLABY pipeline. All sources were inspected
by Tobias Westmeier, and objects deemed to be questionable were deleted. An
example would be an optical galaxy split in two by SoFiA. Over the 3 fields
between 7 and 14% of the sources were eliminated in this way. Half of these
involve pairs or splits. It is customary to exclude such objects from the TFR.
The effects of radio frequency interference are also trapped at this stage.

Table 1 reports the TFR data for the NGC 4808 field. Column (1) is the name of
the WALLABY survey HI detection. Columns (2) & (3) are the SoFiA coordinates
of the WALLABY HI detections. Column (4) is the mean velocity of the HI
profile integrated over the spectrum. Column (5) is the axial ratio of the
DECaLS222https://datalab.noirlab.edu/ls/decals.php $g$ band galaxy image,
which yields the inclination $i$ of the disk. The axial ratio was measured at
approximately 5% of the sky background level with the ellipse task of
IRAF333https://iraf-community.github.io. A minimum axial ratio of 0.2 was
adopted. Zeros denote galaxies for which no axial ratio could be measured.

Coordinates from the HyperLeda catalogue differ from WALLABY coordinates by
7.5${}^{{}^{\prime\prime}}~{}rms$ after 2.5$\sigma$ deviates were removed,
with equal contributions from RA and Dec. The WALLABY beam diameter is
30${}^{{}^{\prime\prime}}$ and this is a contributor444 Typical position
uncertainties for HI point sources in WALLABY are estimated as the beam
diameter (30") divided by the source signal-to-noise, resulting in 7.5$"$
uncertainty only for 4$\sigma$ detections. Westmeier et al. (2022) found an
$rms$ of 5${}^{{}^{\prime\prime}}$ in the phase 1 pilot survey. In some cases
there may also be a difference between the HI centroid and the centroid of the
stellar light. Columns (6) & (7) are the WISE555Wright et al. (2010) W1 total
galaxy magnitude after removal of contaminating stars and its uncertainty.
Columns (8) & (9) are the width at half peak (or double peak) of the HI
profile and its uncertainty. Column (10) is the signal to noise ratio of the
HI profile. Column (11) provides other names for the source from the HyperLeda
catalogue. Double identifications were eliminated by choosing the closer of
the two galaxies. In the TFR we use Wmx, the width after correction for
resolution and turbulence following Tully & Fouqué (1985). The velocity axis
of the TFR is $\Delta{\rm V(0)~{}=~{}Wmx~{}/~{}sin}~{}i~{}/\rm{(1+z)}$, where
$i$ is obtained from column (5)’s optical axial ratio. Nineteen galaxies have
Wmx both measured from WALLABY and compiled by Tully et al. (2009, EDD, the
Extragalactic Distance Database) and Courtois et al. (2009). The mean velocity
width ratio, EDD/WALLABY, is 1.00 $\pm$ 0.01, and the $\chi^{2}$ per degree of
freedom for the identity relation is 0.27, indicating that for these bright
galaxies the velocity width uncertainties have been overestimated. The
velocity structure of the NGC4808 field is shown in Figure 1. Some groups and
filaments of galaxies are visible.

###  2.1 Comparison with Arecibo observations

Only a small portion of the WALLABY footprint protrudes into the northern
hemisphere. The NGC 4808 field therefore provides a rare opportunity to
compare observations with those obtained by the Arecibo Observatory in the
ALFALFA Survey (Haynes et al. 2018) and catalogued in EDD and labelled Wmx1.
Figure 2 shows this comparison.

Figure 2: (a) Comparisons of velocity widths from Table 1 and those from
ALFALFA.

Figure 2: (b) A = ALFALFA, W = WALLABY. The vertical axis essentially shows
the difference between WALLABY and ALFALFA velocity widths.

The measured redshifts of WALLABY and Arecibo are in good agreement. Although
6% of the velocity widths are in disagreement by more than twice the joint
uncertainty, this is no more than expected statistically. We note the more
extreme cases, WALLABY J125258+073025, WALLABY J130412+43057, WALLABY
J130012+054417 and WALLABY J130950+062601. Examination of the HI profiles of
the discrepant galaxies reveals that both their WALLABY and ALFALFA profiles
are of low signal to noise (S/N)and they are all distant, cz $>$ 10,000 km
s-1. Another way of looking at this comparison is in the lower section of
Figure 2. Here the $hyperfit$ slope is significant, –0.072 $\pm$ 0.006.

###  2.2 TFR for the NGC 4808 field

The galaxy inclinations are calculated in the normal way

$\cos^{2}i=\frac{(b/a)^{2}-0.2^{2}}{1-0.2^{2}}$ $None$

where $b/a$ is the axial ratio. The minimum axial ratio of 0.2 has been
adopted since the original work of Tully & Fisher (1977). Paturel et al.
(2003) listed no galaxies with $b/a~{}<$ 0.25 in their Principal Galaxies
Catalogue. In $\S$A4 we note that we see exceptions with $b/a~{}<$ 0.2, but
these are recorded in Table 1 as $b/a$ = 0.2. This is not an issue, as they
are clearly edge-on. We use the data of Table 1 to construct the TFR. Excluded
from Figure 3 are galaxies with inclinations less than 45∘ for which sin $i$
is too uncertain, those with velocity width errors greater than 20 km s-1, and
those with S/N $<$ 3.7. Absolute magnitudes were calculated with a Hubble
Constant of 73 km s-1Mpc-1 (Riess et al. 2022) after correction of
heliocentric velocities to the cosmic microwave background frame, following
Lineweaver et al. (1996). A simple least squares linear fit to Figure 3,
excluding the outlier WALLABY J130436+045341 and 3 other 2.5$\sigma$ deviates,
gives a $\chi^{2}$ per degree of freedom of 5.1, its difference from unity
indicating that the velocity width uncertainties are partially responsible for
the scatter in the TFR, but there is intrinsic scatter as well. In $\S$4.2 we
quantify the uncertainties in $i$ which contribute 0.53 mag to the vertical
errors, compared with 0.46 mag for the width uncertainties here. By comparison
errors in W1 are negligible, growing slowly from 0.01 to 0.1 mag going from 14
to 17 mag in W1. We explore possible ways to reduce the uncertainties in $i$
in the Appendix. A similar $\chi^{2}$ is obtained from a fit with the hyperfit
Bayesian regression package (Robotham & Obreschkow 2015), including an assumed
Gaussian scatter of 200 km/s from peculiar velocities. Hyperfit maximizes the
likelihood of a linear fit in the presence of uncertainties in both
coordinates. This is an important distinction from a least squares fit, when
there is a range of errors in the data. Unbiased estimators for the population
model of the vertical scatter and its variance can be obtained. The website
interface to Hyperfit was accessed at hyperfit.icrar.org. The intrinsic
scatter in the TFR measured by hyperfit is 0.85 mag. Selection biases may also
affect the fit, but these are not investigated here

Figure 3: TFR for the NGC4808 field. The dashed line is the best unweighted
linear fit; the green line is the result from hyperfit, which weights the
fitted points by their uncertainties and allows for intrinsic scatter. The
blue line is the TFR of Bell et al. (2023).

Photometry for galaxies with names in column (11) of Table 1 is also available
from the Siena Galaxy Atlas (Moustakas et al. 2023). This is presented in the
Appendix.

###  2.3 Star formation

The W1 WISE bandpass has some sensitivity to PAH emission (Cluver et al. 2017)
and so we have examined the W1–W2 colour in this sample. Figure 4 shows that
the vast majority of these HI detections has W1–W2 $<$ 0.2 mag, making it
unlikely that there is a significant number of starburst galaxies in the
sample. We have located galaxies with W1–W2 $>$ 0.25 mag in the TFR of Figure
3 and only one of them, WALLABY J130903+065753 is significantly discrepant in
the TFR (on the high luminosity side.) It may be a starburst galaxy.

Figure 4: Distribution of W1–W2 colours for the galaxies in Table 1 (blue).
The Vela and NGC 5044 fields are shown in red and black respectively. Vela and
NGC 4808 have been upscaled by a factor of 3 for ease of comparison

###  2.4 Baryonic TFR

For galaxies with a large HI mass relative to their stellar mass it stands to
reason that adding it to the stellar mass will make a good alternative TFR
(McGaugh et al. 2000). For our sample the HI mass is a product of the template
science code666carnaby.aussrc.org:/mnt/shared/wallaby/notebooks/WALLABY_
notebooks/user_science.ipynb run after the SoFiA pipeline and correction for
the WALLABY flux deficit, and the stellar mass in solar masses can be
calculated from

$\log M_{*}=-0.04+1.12~{}\log\rm{L}_{\rm{W1}}$ $None$

(Wen et al. 2013), where LW1 is the 3.4$\mu$ luminosity in solar units. We
also considered the stellar mass formula of Cluver et al. (2014).That formula
gives a stellar mass larger by a factor 1.42$\pm$0.02 than Wen’s, and we have
not used it because the uncertainties in WISE W2 are 50% larger than in
W1777The procedure described in the Appendix makes this choice moot in the use
of the BTFR for CosmicFlows4.. The HI mass is multiplied by 1.3 to account
approximately for other species (McGaugh et al. 2021), and corrected to the H0
value used for M∗. Figure 5 is the baryonic TFR for galaxies with cz $<$
10,000 km s-1. With four 2.5$\sigma$ deviates removed, the scatter about the
linear least squares fit and about the $hyperfit$ is 0.25 dex or 0.63 $\pm$
0.14 mag, compared with 0.65 $\pm$ 0.13 mag for the W1 TFR. Although the
baryonic TFR is an alternative to the W1 TFR, it seems to be equal, rather
than superior, for the purposes of measuring peculiar velocities.

Figure 5: Baryonic TFR for galaxies in the NGC 4808 field with cz $<$ 10,000
km s-1. The vertical axis is the sum of stellar and gas masses. The black line
has slope 4. The green line is the $hyperfit$ with slope 4.45 $\pm$ 0.29. The
blue line is from Lelli et al. (2019).

##  3 TFR for the Vela field

Table 2 contains the optical, infrared and radio data for the Vela field,
centred on 10h 3m and –45d 36m, and has the same format as Table 1. The
structure of this field is shown in Figure 6, strengthened by redshifts from
the overlapping region of the MeerKAT Vela supercluster survey (Rajohnson et
al. (2024), and the TFR for the field with S/N $>$ 3 is shown in Fig 7. We
dropped the S/N threshold from that used in the previous field because of the
smaller number of galaxies available. The vertical scatter for a linear fit
excluding the lowest velocity width galaxy WALLABY J095710-485624, which is an
outlier, is 0.86 mag. Although the Vela field is at low Galactic latitude
(–8∘), it proved possible to measure accurate W1 total magnitudes by removing
superposed stars. The field is close to the centre of the Laniakea
Supercluster (Tully et al. 2014), and will be of importance in the study of
the velocity field in this region. We defer this to a future study when
adjacent fields can be included.

Figure 6: WALLABY Vela galaxies in the supergalactic plane. The long axis is
the heliocentric recession velocity in the SGY direction, the vertical axis,
the SGX direction. The dynamically significant Vela Supercluster identified by
Kraan-Korteweg et al. (2017) and Courtois et al. (2019) is visible at 18,000
km s-1within WALLABY’s range. Redshifts from Table 2 are solid symbols,
MeerKAT redshifts (Rajohnson et al. 2024) are open symbols and published and
forthcoming optical Vela redshifts are plus signs. Figure 7: TFR for the Vela
field. The green line is the $hyperfit$.

##  4 The NGC 5044 field

Figure 8: WALLABY galaxies from the NGC 5044 field in the supergalactic plane.
The long axis is the heliocentric recession velocity in the SGY direction. The
vertical axis is the SGX coordinate.

This field is the largest of the pilot survey at 120 square degrees. Its
structure is shown in Figure 8. The WALLABY and WISE data are in Table 3,
which has the same format as Table 1, and the TFR is Figure 9. Where the
galaxy seemed too round to warrant ellipse fitting, a zero appears in the
axial ratio column of Table 3. Zeros were also recorded in the fairly rare
case that the source was just outside the boundaries of the closest DECaLS
image. Comparison with published data from Nancay, Greenbank and Parkes (Tully
et al. 2009, EDD, Springob et al. 2005, Theureau et al. 2006, and Koribalski
et al. 2004) is in Tables 4 and 5 and Figures 10 and 11, which compare WALLABY
velocities with published velocities and WALLABY velocity widths with
published velocity widths, respectively. Where there are two published HI
profiles, both are plotted in the figures. The last two columns of these
tables are the WALLABY values from Table 3.The comparison is good. With the 3
most deviant points in Figure 11 removed, there is an offset of 2 $\pm$ 2 km
s-1from the dashed line. The velocity widths in Tables 4 & 5 and Figures 10 &
11 have not been corrected for resolution and turbulence.

Figure 9: TFR for the NGC5044 field. Fourteen 3$\sigma$ deviates from the
regression line have been removed. Only two of these are starburst candidate
galaxies with W1 – W2 $>$ 0.25 mag. Magnitude error bars are mostly
vanishingly small. The green line is the $hyperfit$. There is a skew
distribution around the fit, but this does not seem to be related to unusual
redshifts or inclinations. Figure 10: Comparison of WALLABY velocities from
Tables 4 and 5 in the NGC 5044 field with published heliocentric velocities.

Figure 11: Comparison of WALLABY velocity widths from Tables 4 and 5 in the
NGC 5044 field with velocity widths compiled in EDD (Tully et al. 2009). The
dashed line is the 1:1 line. Below: The difference plot with the 3 most
deviant points removed.

The fitted TFRs in our three WALLABY fields are similar to one another within
the errors.

Fu (2024) has developed a Lucy rectification algorithm for cases where axial
ratios are highly uncertain, which produces a TFR based on the statistical
distribution of galaxy inclinations. We applied this algorithm to the NGC 5044
field, as it offered by far the largest sample. One starts with an initial un-
inclination-corrected (MW1, W50) plane, and the algorithm then converges and
reduces the scatter. However, the scatter in the final statistical TFR
obtained was 1.79 mag rms, compared with 1.08 mag in Figure 9 with the
$\sin~{}i$ term included. Although it would save a lot of painstaking
measurements with uncertainties that are not well characterized, we elected
not to use this algorithm. Axial ratio information is valuable for WALLABY TFR
data.

###  4.1 HyperLeda diameters

The Principal Galaxies Catalogue (Paturel et al. 1992, PGC) is a very good
match to WALLABY source lists with 1173 out of 1672 sources with PGC or other
bright galaxy names in Tables 1–3 (70%). Paturel et al. (2003) have measured
diameters and axis ratios on the RC2 system (de Vaucouleurs et al. 1976) at a
limiting surface brightness of 25 B magnitudes per arcsec2. A related 21 cm
galaxy scaling relation to the TFR is that between diameter and velocity
width. PGC galaxies have D25 and R25 in HyperLeda (Makarov et al. 2014), and
so the diameters can be corrected to uniform face-on surface brightness by a
prescription in the RC2. For a Hubble Constant of 73 km s-1Mpc-1 the relation
is shown in Figure 12. The scatter in the relation is 0.18 dex, which is
equivalent to 0.9 mag in the standard candle version of the TFR, since
$\delta$d/d = (ln 10)$\delta\log$D, where d is distance and D is diameter,
whereas 2$\delta$d/d = 0.4(ln 10)$\delta$m, where m is magnitude.
Nevertheless, the diameter relation is competitive in this context, and opens
the possibility of using both luminosity and diameter information along with
velocity width. That would be analogous to the Fundamental Plane for early-
type galaxies. $Hyperfit$ reports a significant correlation between diameter
and axial ratio uncertainty, in the sense that the largest physical diameter
galaxies have 0.14 larger R25 uncertainties than those ten times smaller, but
this would not888A change of 0.14 in R25 of 0.14 only makes a difference of 2
degrees in inclination on average. seem to act to suppress the scatter in
Figure 12. If the luminosity TFR and the diameter TFR are used jointly as they
stand, however, errors in velocity width and inclination will produce errors
in distance that correlate.

Figure 12: The relation between PGC diameter and inclination corrected
velocity width for the NGC5044 field. A Hubble constant of 73 km s-1Mpc-1 was
adopted. The green line is the $Hyperfit$.

###  4.2 Kinematic inclinations

Deg et al. (2022) and Murugeshan et al. (2024) have made kinematic maps,
including rotation curves, of many WALLABY galaxies, 108 of which are in the
present work. In this work the inclinations of two flat disk models (FAT and
3DBAROLO) are averaged together and the uncertainty is set to half the
difference between the two fits. In the flat disk algorithm geometric
parameters are averaged across all radii. We have matched those with the
galaxies in Tables 1–3 and the comparison of inclinations is shown in Figure
13. The solid correlation gives us confidence in our ellipse fitted axial
ratios. There is also a good correlation between the axial ratios in Table 3
and HyperLeda axial ratios (Figure 14). If we assume the inclinations derived
from Table 3 have an uncertainty of 12.5 degrees, we obtain $\chi^{2}$ = 1 in
a 1:1 fit. There is no significant offset between kinematic and axial ratio
inclinations down to the 1 degree level. Further discussion of axial ratios is
in the Appendix.

Figure 13: Inclinations from WALLABY kinematic modelling (Deg et al. 2022) and
those used here from ellipse fitting. The latter have not had uncertainties
measured. The green line is equality. Figure 14: Axial ratios from HyperLeda
for PGC galaxies and those used here from ellipse fitting. The line is the 1:1
line.

###  4.3 I and J magnitudes

An additional resource is the DECam Local Volume Exploration Survey (DELVE DR2
catalog, Drlica-Wagner et al. 2022). We explore this because W1 total
magnitudes may not be available for the volume of data generated by the full
WALLABY survey. To reduce multiple matching, PGC positions were used, and cuts
were made to SExtractor parameters (Bertin & Arnouts 1999) semi-major axis
($>$ 5 arcsec), $g$ magnitude ($<$ 19) and positional error $<$ 15 arcsec.
Where multiple matching occurred, the closest galaxy to the PGC position was
taken to be the match. Inspection of the DECaLS images confirmed that this is
an effective procedure in finding the galaxy that is most likely to be the HI
source. A TFR is shown in Figure 15, where the $i$ magnitude is mag_auto_i and
the axial ratio is b_image_g/ a_image_g. The correlation is strong, as seen in
Table 6, where the hyperfit $\chi^{2}$ is shown. The $rms$ difference in
inclinations between DELVE and Table 3 is 15 degrees, similar to what was
found in the previous section, with DELVE delivering a slightly better
$\chi^{2}$. With 2.5$\sigma$ deviates rejected, the vertical scatter is 1.27
mag.

Figure 15: TFR from DELVE DR2 $i$ magnitudes for galaxies with PGC positions
in the NGC 5044 field. The error bar is an average velocity width uncertainty
and a peculiar velocity uncertainty of 200 km s-1. The line is the TFR of
Springob et al. (2018).

Armed with accurate positions from HyperLeda and DELVE, we can perform a match
with a catalogue of galaxy magnitudes prepared for the 4MOST collaboration
(Taylor et al. 2023) and based on the VISTA Hemisphere Survey. We present the
J-band TFR in Figure 16. The vertical scatter is 1.45 mag. Also available from
HyperLeda are I magnitudes from the DENIS survey (Paturel et al. 2005). Figure
17 shows this TFR, and its vertical scatter is 0.81 mag. This catalogue covers
the southern hemisphere with cutouts for the Magellanic Clouds and low
Galactic latitudes. The $\chi^{2}$ per degree of freedom for these four TFRs
is given in Table 6. The TFR for the DENIS data is well fit by equation (14)
of the SFI++ sample of Springob et al. (2018). The magnitude extinction
correction (1.05 $\log(a/b)$ ) of Giovanelli et al. (1994) does not change
$\chi^{2}$ significantly. We provide slopes and zeropoints of the $hyperfits$
in Table 8, but note that these quantities will be determined with larger
samples in the full WALLABY survey.

Figure 16: TFR in J magnitudes from 4HS (the 4MOST Hemisphere Survey) for the NGC 5044 field. The error bar shows an average velocity width uncertainty. Figure 17: TFR in I magnitudes from the DENIS survey for the NGC 5044 field. The dashed line is from Springob et al. (2018). Figure 19: A portion of the NGC 5044 field in real space, where the Z coordinate is in the radial direction, and the tangential coordinates point N (Y) and E (X). The difference between the TFR distance times H0 and the redshift is the peculiar velocity, shown by the length of the arrows. Red is redshift and blue is approaching. These have been scaled down by a factor of ten for clarity. A bulk flow of 500 km s-1depicted by the barely visible green arrow in the foreground, added to these data can be retrieved, as described in $\S$5.2. Table 6: TFR Quality of linear fit, NGC 5044 field TFR | Source | Figure | S/N cutoff | $\chi^{2}$ | n
---|---|---|---|---|---
$i$ mag | DELVE DR2 | 15 | none | 1.48 | 325
J mag | 4MOST | 16 | 3.7 | 5.34 | 189
I mag | DENIS | 17 | 3.0 | 3.30 | 303
W1 mag | WISE | 9 | 3.7 | 3.20 | 344
Linear fits were used, not $hyperfits$.

The $\chi^{2}$ was calculated with an intrinsic TFR scatter of 0.40 mag
(Masters et al. 2014) and an assumed inclination error of 12.5 degrees (see
below). The photometric uncertainties in DELVE and 4MOST are included but are
negligible.

###  4.4 WALLABY detections with no optical counterpart

In Tables 1-3 WALLABY pilot survey galaxies not detectable in WISE or DECaLS
and free from close companions are a fraction of a percent of the total. In a
sample of 1700 galaxies statistical juxtaposition of noise in the datacubes
will occur, and, although all SoFiA detections have been examined,
confirmation is needed. Deeper optical imaging and higher resolution HI maps
are desirable for these objects. These sources extend over multiple WALLABY
beams, so the velocity range is not smeared out. They are being studied
intensively in another WALLABY program (O’Beirne et al. 2024), and thus we
shall not go into detail here. Their relationship to those Ultra Diffuse
Galaxies (UDGs; Mancera Pina et al. 2019, 2020), which are not HI rich (For et
al. 2023) remains to be explored.

##  5 Discussion

###  5.1 Combined fields

We combine the TFRs for the three fields in Figure 18. The intercepts of the
three TFRs are not different within the uncertainties. According to the IRSA
dust map viewer the Schlafly & Finkbeiner (2011) extinction in Vela varies
from E(B-V) = 0.17 mag in the NE region of our field to 0.475 mag in the SW.
In the W1 bandpass this range is (0.037, 0.103) mag in AW1. This is not
responsible for the scatter in Figure 7 or Figure 19. The other two fields are
high latitude fields with E(B-V) = 0.03 and 0.06 mag.

###  5.2 A simulation

The full WALLABY survey will address the growth of structure in the Universe,
measuring $f\sigma_{8}$ with high statistical accuracy (Said et al. 2020) and
discovering large scale flows in the accessible volume. As a simple test we
inserted a 500 km s-1bulk flow in a 104 Mpc3 volume of the NGC 5044 field at
5500 km s-1redshift, as depicted in Figure 20. Scatter of 1.04 mag rms from
the (W1, $\Delta V(0)$) TFR was added to the Hubble flow and the input flow
velocity was recovered with 2.5$\sigma$ significance from 156 galaxies. This
bodes well for the full survey and suggests that expectations based on the
simulations of Boubel et al. (2024) with 7341 ALFALFA galaxies will be
realised. The average TFR scatter assumed in their error model for these 156
galaxies was 0.93 mag.

The full WALLABY survey will cover regions of high and low extinction, and
therefore the W1 magnitudes have a significant advantage for measuring
peculiar velocities on large scales. If these measurements can be automated
for $\sim$105 galaxies, this approach would be preferred. If not, Table 6
suggests that DELVE DR2 would provide a good alternative, better still if that
can be combined with an extinction map to correct the I magnitudes and a
higher throughput filter on the DELVE survey than the PGC catalogue to ensure
unique matching.

Figure 19: The three WALLABY phase 2 pilot survey TFR relations combined.
NGC5044 is in black, Vela is in red and NGC4808 in green.

###  5.3 New positions of the Great Attractor and Vela from the WALLABY
addition to CosmicFlows4

Figure 20 shows comparatively a map of the Norma region as seen from the
computation of the linear velocity field and corresponding density field,
thanks to peculiar velocities (Courtois et al. 2023). The left panel shows the
reconstruction with CosmicFlows4 (CF4) galaxies only (black dots) while the
right panel shows the reconstruction with the WALLABY pilot data added
(coloured dots) to CF4. Before the addition of WALLABY data the Great
Attractor was located a bit closer to us at SGX-SGY=(-30,0) Mpc/h. The new
location is at SGX-SGY=(-40,+10) Mpc/h (see Tables 7a&b). The signal to noise
of the Linear density field reconstruction at the Great Attractor location is
a strong 15$\sigma$. We also note that the velocity flow around Coma cluster
is modified. Now Coma appears as a clearly detached cluster.

This figure corresponds to the Great Attractor position in the Supergalactic
plane SGX-SGY. It is a slice of $\pm$5 Mpc/h thickness, centred at
supergalactic SGZ= 0 Mpc/h. The blue and red background colors show the linear
density field recovered from the CosmicFlows4 compendium of peculiar
velocities (Courtois et al. 2023). The black dots are galaxies from the
CosmicFlows4 catalogue. The coloured dots are the WALLABY pilot data. Also the
velocity flow around Coma is modified. Now Coma appears as a clearly detached
cluster. This figure corresponds to the Vela supercluster position in the
Supergalactic plane SGY-SGZ. It is a slice of $\pm$5 $i.e.$ 10 Mpc/h
thickness, centered at supergalactic SGX= -130 Mpc/h. The blue and red
background colours show the linear density field recovered from the
CosmicFlows4 compendium of peculiar velocities (Courtois et al. 2023). The
green square is the position of Vela as found by Kraan-Korteweg et al. 2017
from redshift surveys. The red triangle was the position of Vela as found by
Courtois et al. 2019 using the V-web of CF3. The black dots are galaxies from
the CosmicFlows4 catalogue. The coloured dots are the WALLABY pilot data.

The region scrutinized in Figure 21 is a slice at supergalactic SGX=- 130
Mpc/h. A clear over-density of galaxies is seen on both sides of the zone
obscured by the Milky Way disc (vertical on this figure) at SGZ=-130 Mpc/h.
This is what was named the "Vela wall" of the "Vela supercluster": a filament
running across the ZOA and extending in total to more than 6,000 km s-1from
the redshift surveys’ point of view. The black arrows on this figure
correspond to the peculiar (gravitational) velocity field. A striking result
is that, quite independently, the new WALLABY data confirms the Vela position
published by Kraan-Korteweg et al. (2017). The Vela supercluster extends from
side to side across the ZOA. Since it is a three-dimensional velocity field,
on the figure these vectors are projected onto the plane SGY-SGZ. The red
triangle on this Figure 21, was published in 2019 by Courtois et al. as a
point of convergence of the V-web located at SGX-SGY-SGZ (-13,000; 7,000;
-9,000) km s-1. This location is the central region of a gravitational basin
of attraction located on the sky in the Vela constellation direction. This
Vela large-scale structure is not part of the larger Shapley attractor as one
can see that there is a clear delimitation of the streamlines splitting
between these two basins. Consequently, the cross-analysis of redshift surveys
data (Kraan-Korteweg 2017) and the new addition of WALLABY data in the
southern hemisphere to the peculiar velocity surveys data confirms the
position of the Vela supercluster at SGY-SGZ=(40; -140) Mpc/h. The signal to
noise of the linear density field reconstruction at the Vela location has
strong 4$\sigma$ significance. We also note that before the WALLABY data the
cluster NGC5044 was not well reconstructed by Cosmic-Flows-4 catalogue. Even
worse there was an under-density (a cosmic void) reconstructed at its
location. The addition of the WALLABY pilot data, causes NGC5044 now to appear
on the map at SGY-SGZ=(100;0) Mpc/h.

Table 7: (a) Large scale structure parameters Positions of the Great Attractor
(GA) and Vela supercluster in CF4 alone in black and with the addition of
WALLABY in bold. The radius of the corresponding spherical overdensity is
given in the last column.

Stru- | SGX | SGY | SGZ | overdensity | distance
---|---|---|---|---|---
cture |  |  |  | at the peak | to $\delta$=0
| Mpc | Mpc | Mpc |  | Mpc
| /h | /h | /h |  | /h
GA | -49/-40 | 4/5 | 8/0 | 0.7/0.9 | 30/40
Vela | -130/ | -15/ | -150/ | -0.4/ | 60/60
|  /-130 |  /40 |  /-140 |  /0.5 |

Structure | vx | vy | vz | Vbulk
---|---|---|---|---
| km s-1 | km s-1 | km s-1 | km s-1
Great Attractor | -153/-102 | 42/78 | 52/37 | 206/188
Vela. | 220/-349 | 82/-39 | 252/-83 | 353/394

Table 7: (b) Bulk flow velocities computed within sphere of radius 20 Mpc/h
centere d around GA [-40,5,0] Mpc/h and Vela [-130,40,-140] Mpc/h. The
addition of pilot phase 2 WALLABY data modifies the amplitude and direction of
the velocity field . The CF4 alone values (in black) and strongly modified
when adding WALLABY data (in bold) in the region of Vela supercluster where
the bulk flow changes direct ion towards negative supergalactic X and Z axis
and is enlarged by an amount of 50km/s reaching 394 km s-1 This shows that
Vela is a main gravitational actor in the southern sky large-scale structures.

CosmicFlows4 is the most advanced representation of the flow field of galaxies
within 20,000 km s-1, using redshift independent distances. A multiwavelength
baryonic TFR has been adopted for this purpose, and in the Appendix we
describe the calibration $pro-tem$ of our single wavelength (W1) baryonic TFR,
so that pilot survey distances can be introduced into the CF4 database, and a
new reconstruction run. Reconstruction is the process of calculating the
gravitational field of galaxies with known distances, and thus, in the linear
approximation, the peculiar velocity field. At this stage we are not able to
include WALLABY selection effects in the reconstruction, as we are still
learning what these are. The S/N ratio cutoff of the WALLABY survey is now
known (Westmeier et al. 2022; Murugeshan et al. 2024), which will allow
selection effects to be simulated.

Figure 20: In the left panel is the flow field solution computed with only CF4
data. In the right panel is the solution using distances from CF4 + WALLABY.
WALLABY data points are in colour. The background red shading corresponds to
mass overdensity and blue to relative underdensity. The arrows show the
direction of the consequent flow field. Figure 21: A SGY-SGZ slice at SGX=-130
Mpc/h. Left and right panels are as in the previous figure. The Vela
supercluster is near the ZOA (which is at SGY =0 vertical). The position of
Vela from Kraan-Korteweg et al. (2017) is a green square. And the position of
Vela as a knot of the V-web (Courtois et al. 2019) is a red triangle.

The first plot (Figure 20) is a SGX-SGY slice at SGZ=0. The red blob across
the Zone Of Avoidance (ZOA) (which is horizontal SGY=0) and SGX=-40 Mpc/h is
the Great Attractor. Figure 21 is perpendicular to it. The effect of adding
the WALLABY pilot survey galaxies is to greatly increase the spatial
resolution of the flow field.

Table 8: Summary of data and cuts

Target | Fie- | Area | PDR2 | Table | SNR | incl | used
---|---|---|---|---|---|---|---
group | lds | deg2 |  | tally | cut | cut† | TFR
N4808 | 1 | 30 | 231 | 201 T1 | 3.7 | 96 | 29
Vela | 1 | 30 | 203 | 143 T2 | 3 | 34 | 71
N5044 | 4 | 120 | 1326 | 1238 T3 | 3.7* | 26 | 348
Total | 6 | 180 | 1760 | 1582 |  | 398 | 448
*also a 3$\sigma$ TFR deviates cut |  |
†Numbers cut for $i~{}>~{}45^{\circ}$ |  |

Table 9: $Hyperfits$*

Field | Slope | $\pm$ | $\beta$ | $\pm$ | $\sigma$ | $\pm$
---|---|---|---|---|---|---
|  |  | mag | mag | mag | mag
NGC 4808 Fig 3 | -10.20 | 0.76 | 2.54 | 1.82 | 0.65 | 0.13
Vela Figure 7 | -11.57 | 0.84 | 5.51 | 1.99 | 0.90 | 0.12
NGC 5044 Fig 9 | -10.68 | 0.30 | 3.26 | 0.69 | 0.94 | 0.06
*$M(W1)=\alpha\log\Delta V(0)~{}+~{}\beta$. Slope = $\alpha$; $\sigma$ = scatter.
Columns headed $\pm$ are uncertainties in columns to their left.

##  6 Conclusions

The WALLABY Pilot Survey has taught us a number of things that can be built on
in the full survey, which is now under way.
(1) The TFR is clearly observed in the three fields of the WALLABY Pilot
Survey Phase 2 and can be used for redshift independent distances. A summary
is given in Table 9. There are ten times the number of galaxies in these
fields as there are for these parts of the sky in CosmicFlows4.
(2) Axial ratios of galaxies from isophotal ellipse fitting in the optical
correlate with disk inclinations from WALLABY kinematic modelling and with
HyperLeda axial ratios. The scatter in this relation allows our axial ratio
uncertainties to be estimated, and this comes close to explaining the TFR
scatter we see. Measuring and controlling errors in inclination are crucial to
understanding the scatter in the TFR and estimating distances.
(3) A diameter/velocity-width scaling relation with scatter comparable to the
TFR can be readily constructed from HyperLeda diameters. Further work is
warranted on investigating the origin of this relation and potentially
combining it with the TFR to obtain better distance estimates.
(4) For WALLABY sources matched to PGC galaxies, 4MOST magnitudes based on the
VISTA Hemisphere Survey can be used to make a J magnitude TFR, and DELVE
(DENIS) magnitudes can be used to make an $i$ (I) magnitude TFR. These would
require calibrations before they could be used to investigate cosmic flows. By
calibrations we mean the slope of the TFR and any nonlinearity. The zeropoint
affects Hubble constant determinations, but not peculiar velocities.
(5) A number of optical non-detections have HI properties similar in hydrogen
mass to luminosity ratios seen in one or two extreme objects in the Local
Volume HI Survey of Koribalski (2018). These number $\sim$0.3% of the HI
detections in the NGC 5044 field. Confirmation of these objects is required.
(6) Forecasts for constraints from the full WALLABY survey on the growth rate
of structure at the current epoch and for the measurement of large scale flows
seem sound based on the pilot survey.
(7) Addition of WALLABY galaxies to CosmicFlows4 increases the spatial
resolution of the flow field because the higher sampling density affords more
detail in the reconstruction.

Table 1: WALLABY data and WISE photometry NGC 4808 field Name | RA | Dec | vhelio | b/a | W1 |  $\delta$W1 | W50 |  $\delta$W50 | S/N | alias
---|---|---|---|---|---|---|---|---|---|---
| J2000 |  | km s-1 |  | mag | mag | km s-1 | km s-1 |  |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11)
WALLABY_J124747+042017 | 191.94598 | 4.33818 | 987 | 0.878 | 10.28 | 0.03 | 46 | 18 | 4.2 | NGC 4688
WALLABY_J124805+065910 | 192.02299 | 6.98568 | 13424 | 0.760 | 12.83 | 0.02 | 130 | 19 | 2.1 | PGC043228
WALLABY_J124822+082925 | 192.09509 | 8.49036 | 1011 | 0.666 | 7.35 | 0.01 | 424 | 19 | 2.9 | NGC 4698
WALLABY_J124911+032310 | 192.29604 | 3.38610 | 722 | 0.739 | 9.50 | 0.01 | 167 | 16 | 6.0 | NGC 4701
WALLABY_J124915+043926 | 192.31544 | 4.65741 | 2668 | 0.860 | 12.92 | 0.03 | 75 | 17 | 4.9 | UGC 7976
WALLABY_J124923+050820 | 192.34853 | 5.13909 | 12410 | 0.725 | 13.83 | 0.01 | 212 | 25 | 1.8 | PGC3395349
WALLABY_J124925+042328 | 192.35762 | 4.39118 | 2643 | 0.550 | 13.82 | 0.04 | 104 | 18 | 3.9 | PGC1267592
WALLABY_J124935+033620 | 192.39824 | 3.60573 | 7085 | 0.897 | 12.46 | 0.01 | 166 | 18 | 4.3 | PGC043361
WALLABY_J124937+074725 | 192.40498 | 7.79054 | 16420 | 0.739 | 14.94 | 0.02 | 273 | 19 | 2.0 |
WALLABY_J124944+044608 | 192.43346 | 4.76898 | 8441 | 0.370 | 12.28 | 0.01 | 146 | 19 | 2.6 | PGC043389
WALLABY_J124947+035042 | 192.44933 | 3.84521 | 698 | 0.440 | 13.75 | 0.03 | 35 | 17 | 5.4 | UGC 7983
WALLABY_J124950+025100 | 192.45959 | 2.85022 | 1159 | 0.220 | 9.82 | 0.01 | 208 | 19 | 2.2 | UGC 7982
WALLABY_J124957+040438 | 192.49109 | 4.07742 | 10202 | 0.680 | 13.60 | 0.02 | 218 | 18 | 4.1 | PGC1263188
WALLABY_J124959+054921 | 192.49675 | 5.82272 | 630 | 0.720 | 13.80 | 0.02 | 109 | 18 | 3.3 | PGC1289538
WALLABY_J125012+073442 | 192.55397 | 7.57855 | 11451 | 0.760 | 10.73 | 0.01 | 274 | 19 | 3.1 | AGC225050
WALLABY_J125103+072753 | 192.76622 | 7.46492 | 15171 | 0.640 | 12.37 | 0.01 | 297 | 20 | 2.0 | PGC1322513
WALLABY_J125112+045132 | 192.80307 | 4.85892 | 7532 | 0.884 | 10.18 | 0.01 | 233 | 18 | 3.5 | NGC 4734
WALLABY_J125114+052031 | 192.81215 | 5.34211 | 7514 | 0.977 | 13.45 | 0.02 | 74 | 17 | 4.6 | AGC225201
WALLABY_J125121+063829 | 192.84126 | 6.64150 | 14998 | 0.740 | 14.21 | 0.02 | 124 | 17 | 5.4 | PGC1304685
WALLABY_J125127+054748 | 192.86482 | 5.79682 | 14439 | 0.710 | 12.50 | 0.01 | 455 | 19 | 2.6 | PGC1289326
WALLABY_J125133+080241 | 192.88995 | 8.04494 | 3597 | 0.888 | 13.49 | 0.08 | 130 | 18 | 4.0 | PGC043556
WALLABY_J125134+055147 | 192.89421 | 5.86332 | 14592 | 0.674 | 12.03 | 0.02 | 401 | 24 | 1.8 | PGC1290429
WALLABY_J125156+035954 | 192.98697 | 3.99838 | 7684 | 0.574 | 15.41 | 0.02 | 206 | 28 | 1.7 | PGC1261946
WALLABY_J125211+043045 | 193.04642 | 4.51261 | 19307 | 0.790 | 13.03 | 0.01 | 271 | 19 | 2.6 | PGC4345126
WALLABY_J125215+042728 | 193.06422 | 4.45782 | 696 | 0.570 | 15.42 | 0.11 | 57 | 19 | 2.5 | AGC226122
WALLABY_J125224+071046 | 193.10010 | 7.17953 | 14948 | 0.325 | 13.73 | 0.03 | 230 | 17 | 6.6 | PGC1315615
WALLABY_J125233+031517 | 193.13998 | 3.25474 | 14620 | 0.666 | 12.38 | 0.01 | 295 | 22 | 1.9 | PGC1248106
WALLABY_J125243+075643 | 193.17969 | 7.94529 | 11588 | 0.740 | 13.27 | 0.02 | 201 | 22 | 1.9 | PGC1335032
WALLABY_J125258+073025 | 193.24283 | 7.50694 | 16023 | 0.790 | 12.56 | 0.02 | 421 | 19 | 3.0 | PGC043729
WALLABY_J125303+070944 | 193.26555 | 7.16228 | 15196 | 0.600 | 16.16 | 0.06 | 111 | 19 | 2.3 | PGC5509705
WALLABY_J125308+081035 | 193.28596 | 8.17653 | 14834 | 0.490 | 16.03 | 0.05 | 123 | 41 | 1.1 | PGC434576
WALLABY_J125311+032639 | 193.29700 | 3.44418 | 2789 | 0.900 | 16.54 | 0.20 | 29 | 19 | 2.6 | PGC166147
WALLABY_J125313+042746 | 193.30641 | 4.46279 | 725 | 0.688 | 10.35 | 0.01 | 87 | 16 | 6.2 | NGC 4765
WALLABY_J125334+060947 | 193.39287 | 6.16324 | 13460 | 0.410 | 12.69 | 0.02 | 160 | 19 | 2.5 |
WALLABY_J125339+040434 | 193.41631 | 4.07620 | 887 | 0.710 | 14.69 | 0.04 | 40 | 18 | 3.7 | AGC224229
WALLABY_J125340+064728 | 193.42010 | 6.79115 | 7630 | 0.808 | 11.88 | 0.01 | 206 | 19 | 2.2 | PGC043817
WALLABY_J125341+034603 | 193.42392 | 3.76761 | 19644 | 0.851 | 13.03 | 0.02 | 145 | 19 | 3.0 | PGC1258221
WALLABY_J125343+040920 | 193.43007 | 4.15566 | 772 | 0.825 | 14.74 | 0.05 | 39 | 19 | 2.6 | PGC1264260
WALLABY_J125413+052149 | 193.55656 | 5.36375 | 14499 | 0.544 | 12.01 | 0.01 | 312 | 19 | 2.6 | PGC4676508
WALLABY_J125419+064115 | 193.57948 | 6.68763 | 3633 | 0.785 | 13.64 | 0.01 | 92 | 27 | 1.7 | PGC3091848
WALLABY_J125431+050959 | 193.63210 | 5.16657 | 19563 | 0.604 | 12.72 | 0.01 | 484 | 45 | 1.0 | PGC1279102
WALLABY_J125443+050110 | 193.68056 | 5.01958 | 10661 | 0.533 | 16.33 | 0.08 | 120 | 18 | 3.4 |
WALLABY_J125443+080310 | 193.68300 | 8.05288 | 2520 | 0.715 | 11.23 | 0.01 | 243 | 19 | 3.1 | NGC 4791
WALLABY_J125445+045357 | 193.69009 | 4.89937 | 7453 | 0.650 | 15.17 | 0.06 | 123 | 19 | 2.8 | PGC1274939
WALLABY_J125450+072542 | 193.71011 | 7.42845 | 15011 | 0.617 | 13.43 | 0.01 | 274 | 25 | 1.8 | PGC1321584
WALLABY_J125500+051140 | 193.75122 | 5.19446 | 19741 | 0.790 | 15.73 | 0.03 | 79 | 18 | 4.5 | PGC3480219
WALLABY_J125507+040229 | 193.78165 | 4.04148 | 14467 | 0.972 | 12.04 | 0.01 | 91 | 19 | 2.7 | PGC1262572
WALLABY_J125509+075453 | 193.79150 | 7.91487 | 2655 | 0.551 | 12.18 | 0.02 | 178 | 18 | 3.7 | UGC 8042
WALLABY_J125515+081543 | 193.81377 | 8.26203 | 21390 | 0.850 | 12.30 | 0.01 | 169 | 17 | 4.9 | PGC1343076
WALLABY_J125516+025347 | 193.81685 | 2.89662 | 2803 | 0.664 | 9.59 | 0.01 | 365 | 18 | 3.3 | NGC 4799
WALLABY_J125520+050620 | 193.83734 | 5.10573 | 10706 | 0.548 | 13.85 | 0.02 | 200 | 21 | 1.9 | PGC3480237
WALLABY_J125548+041805 | 193.95232 | 4.30158 | 760 | 0.537 | 8.71 | 0.02 | 269 | 15 | 7.7 | NGC 4808
WALLABY_J125548+045901 | 193.95166 | 4.98387 | 14632 | 0.525 | 12.33 | 0.01 | 430 | 18 | 4.3 | PGC1276334
WALLABY_J125549+040049 | 193.95634 | 4.01383 | 712 | 0.518 | 12.24 | 0.03 | 124 | 17 | 5.5 | UGC 8053
WALLABY_J125556+075542 | 193.98351 | 7.92859 | 12464 | 0.495 | 12.68 | 0.01 | 299 | 34 | 1.4 | PGC4538018
WALLABY_J125603+045202 | 194.01451 | 4.86747 | 1375 | 0.800 | 14.06 | 0.05 | 42 | 17 | 4.5 | PGC5057592
continued in full in MNRAS

Table 2: WALLABY data and WISE photometry Vela field Name | RA | Dec | vhelio | b/a | W1 |  $\delta$W1 | W50 |  $\delta$W50 | S/N |  alias
---|---|---|---|---|---|---|---|---|---|---
| J2000 |  | km s-1 |  | mag | mag | km s-1 | km s-1 |  |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11)
WALLABY_J094317-452105 | 145.82089 | -45.35157 | 5340 | 0.313 | 14.04 | 0.13 | 229 | 17 | 5.7 |
WALLABY_J094325-453019 | 145.85829 | -45.50539 | 12065 | 0.616 | 13.72 | 0.05 | 251 | 18 | 3.7 |
WALLABY_J094333-452200 | 145.89011 | -45.36670 | 18231 | 0.511 | 11.49 | 0.02 | 143 | 19 | 2.6 | PGC527583
WALLABY_J094429-464515 | 146.12170 | -46.75434 | 17251 | 0.499 | 13.55 | 0.05 | 277 | 19 | 2.3 |
WALLABY_J094524-480828 | 146.35260 | -48.14116 | 880 | 0.200 | 14.56 | 0.09 | 75 | 15 | 8.0 |
WALLABY_J094533-462130 | 146.39050 | -46.35859 | 7502 | 0.430 | 15.30 | 0.07 | 114 | 18 | 3.4 | PGC515934
WALLABY_J094613-471709 | 146.55690 | -47.28599 | 14082 | 0.500 | 12.57 | 0.05 | 217 | 18 | 4.3 |
WALLABY_J094622-463856 | 146.59392 | -46.64899 | 2704 | 0.300 | 11.18 | 0.02 | 291 | 16 | 6.7 |
WALLABY_J094723-431306 | 146.84944 | -43.21851 | 5318 | 0.479 | 12.93 | 0.03 | 154 | 32 | 1.7 |
WALLABY_J094814-464424 | 147.05835 | -46.74026 | 17507 | 0.422 | 14.26 | 0.02 | 218 | 17 | 5.7 |
WALLABY_J094819-442224 | 147.08121 | -44.37339 | 18139 | 0.281 | 12.27 | 0.01 | 272 | 35 | 2.0 | PGC538024
WALLABY_J094828-472216 | 147.11841 | -47.37133 | 17106 | 0.470 | 12.35 | 0.01 | 297 | 19 | 2.5 | PGC502430
WALLABY_J094830-464320 | 147.12833 | -46.72243 | 17352 | 0.548 | 14.02 | 0.04 | 249 | 17 | 4.5 | PGC511516
WALLABY_J094840-452959 | 147.16727 | -45.49980 | 13467 | 0.226 | 13.01 | 0.02 | 376 | 19 | 3.1 |
WALLABY_J094854-462741 | 147.22504 | -46.46154 | 17222 | 0.536 | 13.28 | 0.02 | 279 | 19 | 3.2 |
WALLABY_J094855-435404 | 147.23100 | -43.90133 | 19445 | 0.873 | 13.13 | 0.02 | 350 | 17 | 4.6 | PGC543149
WALLABY_J094924-454230 | 147.35231 | -45.70839 | 5284 | 0.378 | 12.88 | 0.03 | 98 | 18 | 4.5 |
WALLABY_J094926-435730 | 147.36195 | -43.95849 | 19448 | 0.859 | 13.61 | 0.02 | 203 | 18 | 4.0 |
WALLABY_J094940-454322 | 147.41983 | -45.72292 | 16372 | 0.290 | 11.68 | 0.01 | 458 | 19 | 2.3 | PGC096455
WALLABY_J094959-481705 | 147.49632 | -48.28491 | 5212 | 0.220 | 12.10 | 0.03 | 270 | 16 | 6.1 | PGC489114
WALLABY_J095019-452605 | 147.57959 | -45.43482 | 12136 | 0.506 | 11.70 | 0.01 | 192 | 19 | 2.2 | PGC309881
WALLABY_J095019-441017 | 147.58247 | -44.17142 | 19387 | 0.864 | 12.99 | 0.02 | 120 | 19 | 2.5 | PGC309880
WALLABY_J095031-461322 | 147.63036 | -46.22299 | 13532 | 0.385 | 16.03 | 0.06 | 220 | 18 | 4.5 | PGC517483
WALLABY_J095053-432902 | 147.72421 | -43.48414 | 2699 | 0.717 | 14.04 | 0.05 | 151 | 31 | 3.8 | PGC548188
WALLABY_J095101-451536 | 147.75775 | -45.26022 | 11295 | 0.274 | 14.65 | 0.05 | 161 | 18 | 4.5 | PGC528651
WALLABY_J095126-452831 | 147.85852 | -45.47532 | 12124 | 0.341 | 13.48 | 0.02 | 269 | 17 | 5.0 | PGC526385
WALLABY_J095131-440121 | 147.88051 | -44.02256 | 13106 | 0.415 | 12.22 | 0.01 | 477 | 19 | 2.5 | PGC028395
WALLABY_J095159-443357 | 147.99901 | -44.56604 | 19297 | 1.000 | 15.02 | 0.03 | 101 | 19 | 2.2 |
WALLABY_J095205-443809 | 148.02348 | -44.63591 | 18041 | 0.536 | 12.68 | 0.01 | 254 | 32 | 1.5 | PGC535167
WALLABY_J095211-464251 | 148.04860 | -46.71441 | 13589 | 0.321 | 13.47 | 0.02 | 294 | 17 | 4.8 | PGC511580
WALLABY_J095234-475517 | 148.14436 | -47.92139 | 17230 | 0.738 | 13.98 | 0.03 | 150 | 15 | 7.3 |
WALLABY_J095239-470647 | 148.16661 | -47.11310 | 1820 | 0.900 | 13.03 | 0.07 | 73 | 19 | 2.0 | PGC506395
WALLABY_J095244-474722 | 148.18340 | -47.78953 | 5390 | 0.390 | 13.92 | 0.10 | 115 | 18 | 3.6 | PGC495718
WALLABY_J095311-451624 | 148.29988 | -45.27333 | 11263 | 0.762 | 13.69 | 0.04 | 206 | 19 | 3.1 | PGC528542
WALLABY_J095316-431054 | 148.31738 | -43.18174 | 18933 | 0.600 | 14.28 | 0.02 | 89 | 22 | 1.9 |
WALLABY_J095347-455759 | 148.44792 | -45.96661 | 7089 | 0.200 | 11.14 | 0.01 | 367 | 19 | 2.4 | PGC028528
WALLABY_J095354-433845 | 148.47746 | -43.64592 | 7727 | 0.432 | 14.19 | 0.03 | 175 | 17 | 4.8 |
WALLABY_J095423-443318 | 148.59874 | -44.55511 | 10029 | 0.853 | 13.65 | 0.04 | 150 | 18 | 3.5 | PGC536076
WALLABY_J095433-440456 | 148.63873 | -44.08222 | 17770 | 0.948 | 13.77 | 0.02 | 270 | 19 | 2.8 |
WALLABY_J095441-440640 | 148.67125 | -44.11118 | 17882 | 0.483 | 12.71 | 0.02 | 252 | 19 | 2.3 | PGC540776
WALLABY_J095448-462159 | 148.70078 | -46.36654 | 7074 | 0.824 | 12.91 | 0.02 | 186 | 17 | 5.0 | PGC515876
WALLABY_J095449-461903 | 148.70421 | -46.31764 | 16160 | 0.721 | 14.67 | 0.04 | 275 | 19 | 2.4 | PGC516415
WALLABY_J095457-480416 | 148.73886 | -48.07116 | 11541 | 0.561 | 11.82 | 0.02 | 440 | 18 | 3.5 | PGC308536
WALLABY_J095532-443931 | 148.88661 | -44.65867 | 18673 | 0.799 | 11.88 | 0.01 | 336 | 18 | 3.5 | PGC534960
WALLABY_J095552-455731 | 148.96976 | -45.95863 | 12425 | 0.781 | 14.85 | 0.04 | 93 | 18 | 4.0 |
WALLABY_J095558-472929 | 148.99477 | -47.49157 | 19141 | 0.933 | 14.40 | 0.02 | 120 | 15 | 7.9 |
WALLABY_J095635-453219 | 149.14613 | -45.53882 | 13794 | 0.531 | 14.43 | 0.03 | 174 | 18 | 3.8 |
WALLABY_J095648-450253 | 149.20219 | -45.04817 | 19190 | 0.438 | 15.53 | 0.04 | 228 | 19 | 2.3 |
WALLABY_J095710-485624 | 149.29468 | -48.94017 | 3727 | 0.250 | 12.83 | 0.04 | 40 | 16 | 6.5 | PGC580713
WALLABY_J095719-465024 | 149.32941 | -46.84004 | 13024 | 0.617 | 13.56 | 0.02 | 277 | 19 | 3.1 |
WALLABY_J095802-444730 | 149.51060 | -44.79173 | 23768 | 0.729 | 14.67 | 0.02 | 244 | 36 | 3.7 | PGC533495
WALLABY_J095809-472057 | 149.54031 | -47.34937 | 3644 | 0.896 | 14.38 | 0.05 | 124 | 17 | 5.6 |
WALLABY_J095813-430817 | 149.55484 | -43.13825 | 7307 | 0.396 | 14.88 | 0.06 | 184 | 18 | 3.9 |
WALLABY_J095824-433328 | 149.60017 | -43.55786 | 18236 | 0.608 | 12.85 | 0.01 | 130 | 19 | 2.1 | PGC547363
WALLABY_J095836-470454 | 149.65350 | -47.08191 | 3628 | 0.412 | 10.89 | 0.01 | 109 | 19 | 3.2 |
WALLABY_J095848-455156 | 149.70287 | -45.86573 | 3664 | 0.598 | 12.09 | 0.01 | 196 | 18 | 4.0 |
Continued in full in MNRAS

Table 3: WALLABY data and WISE photometry NGC 5044 field Name | RA | Dec | vhelio | b/a | W1 |  $\delta$W1 | W50 |  $\delta$W50 | S/N | alias
---|---|---|---|---|---|---|---|---|---|---
| J2000 |  | km s-1 |  | mag | mag | km s-1 | km s-1 |  |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11)
WALLABY_J125700-171910 | 194.25180 | -17.31950 | 3972 | 0.620 | 11.65 | 0.01 | 220 | 19 | 2.6 | PGC044234
WALLABY_J125706-182159 | 194.27628 | -18.36646 | 16185 | 0.706 | 11.29 | 0.01 | 88 | 29 | 1.6 | ESO575-036
WALLABY_J125757-130339 | 194.48877 | -13.06087 | 5022 | 0.556 | 9.53 | 0.01 | 215 | 19 | 2.8 | NGC4838
WALLABY_J125834-164819 | 194.64464 | -16.80551 | 3843 | 0.386 | 13.61 | 0.01 | 147 | 19 | 3.1 | PGC044478
WALLABY_J125836-161333 | 194.65154 | -16.22606 | 5266 | 0.000 | 12.41 | 0.01 | 131 | 19 | 2.7 |
WALLABY_J125843-170913 | 194.67995 | -17.15386 | 8361 | 0.485 | 12.88 | 0.01 | 318 | 19 | 2.6 | PGC044499
WALLABY_J125848-114647 | 194.70290 | -11.77985 | 4849 | 0.200 | 13.61 | 0.02 | 154 | 19 | 2.2 | PGC104987
WALLABY_J125850-145324 | 194.71039 | -14.89014 | 4874 | 0.330 | 14.38 | 0.02 | 144 | 18 | 4.1 | PGC918593
WALLABY_J125855-142319 | 194.73131 | -14.38869 | 19381 | 0.000 | 19.04 | 0.46 | 148 | 18 | 3.4 |
WALLABY_J125859-135141 | 194.74915 | -13.86140 | 4883 | 0.496 | 15.01 | 0.02 | 55 | 19 | 2.1 | PGC932206
WALLABY_J125907-121329 | 194.77928 | -12.22482 | 1312 | 0.430 | 13.37 | 0.03 | 80 | 16 | 6.0 | PGC044549
WALLABY_J125910-161749 | 194.79179 | -16.29707 | 12931 | 0.686 | 13.15 | 0.02 | 180 | 19 | 3.0 | PGC899955
WALLABY_J125912-182326 | 194.80096 | -18.39075 | 15297 | 0.000 | 14.13 | 0.01 | 89 | 19 | 2.1 | PGC868681
WALLABY_J125912-124101 | 194.80396 | -12.68385 | 3875 | 0.389 | 14.65 | 0.03 | 134 | 17 | 4.5 | PGC949183
WALLABY_J125923-120455 | 194.84590 | -12.08215 | 6349 | 0.460 | 12.24 | 0.01 | 191 | 18 | 4.5 | PGC3082105
WALLABY_J125930-135159 | 194.87573 | -13.86649 | 13996 | 0.000 | 13.58 | 0.01 | 97 | 18 | 3.4 | PGC932150
WALLABY_J125930-180055 | 194.87677 | -18.01554 | 4959 | 0.430 | 15.59 | 0.06 | 120 | 17 | 4.6 | PGC873976
WALLABY_J125930-120652 | 194.87744 | -12.11468 | 6387 | 0.960 | 12.91 | 0.01 | 129 | 17 | 4.7 | PGC957468
WALLABY_J125931-140755 | 194.87987 | -14.13200 | 6451 | 0.759 | 11.50 | 0.01 | 145 | 17 | 4.9 | NGC4862
WALLABY_J125932-182203 | 194.88594 | -18.36763 | 15110 | 0.603 | 13.85 | 0.02 | 119 | 17 | 4.9 |
WALLABY_J125932-151419 | 194.88669 | -15.23881 | 1418 | 0.571 | 12.78 | 0.01 | 95 | 19 | 2.1 | PGC3082108
WALLABY_J125939-145813 | 194.91435 | -14.97029 | 4953 | 0.221 | 10.80 | 0.01 | 360 | 17 | 5.2 | PGC044645
WALLABY_J125940-151600 | 194.91905 | -15.26692 | 4860 | 0.914 | 13.54 | 0.01 | 97 | 19 | 2.7 | PGC913440
WALLABY_J125942-140140 | 194.92767 | -14.02790 | 4368 | 0.466 | 10.64 | 0.01 | 462 | 18 | 3.6 | NGC4863
WALLABY_J125942-164952 | 194.92847 | -16.83133 | 1368 | 0.450 | 15.81 | 0.07 | 43 | 18 | 4.2 |
WALLABY_J125943-150804 | 194.93118 | -15.13447 | 13409 | 0.945 | 15.41 | 0.05 | 86 | 19 | 2.5 | PGC915253
WALLABY_J125945-145159 | 194.93814 | -14.86639 | 2659 | 0.398 | 13.20 | 0.01 | 147 | 19 | 2.7 | PGC918920
WALLABY_J125949-200826 | 194.95747 | -20.14056 | 13972 | 0.000 | 14.17 | 0.02 | 52 | 29 | 1.6 |
WALLABY_J125951-150446 | 194.96494 | -15.07954 | 12208 | 0.676 | 13.05 | 0.02 | 271 | 18 | 3.4 | PGC916026
WALLABY_J125956-192430 | 194.98334 | -19.40843 | 826 | 0.360 | 14.48 | 0.03 | 45 | 16 | 6.7 | PGC044681
WALLABY_J125959-143124 | 194.99905 | -14.52352 | 2576 | 0.247 | 13.79 | 0.01 | 67 | 17 | 4.7 | PGC923490
WALLABY_J130004-154055 | 195.01862 | -15.68214 | 1135 | 0.200 | 14.47 | 0.05 | 121 | 18 | 3.3 | PGC907834
WALLABY_J130004-152151 | 195.02060 | -15.36439 | 1589 | 0.200 | 10.74 | 0.01 | 117 | 18 | 4.3 | PGC044701
WALLABY_J130010-130042 | 195.04393 | -13.01183 | 4735 | 0.201 | 11.64 | 0.01 | 166 | 19 | 2.6 | PGC044718
WALLABY_J130016-170140 | 195.06892 | -17.02799 | 4908 | 0.416 | 11.14 | 0.01 | 240 | 19 | 3.0 | PGC170439
WALLABY_J130017-122041 | 195.07176 | -12.34494 | 1581 | 0.596 | 11.20 | 0.01 | 168 | 16 | 6.1 | PGC044735
WALLABY_J130018-115758 | 195.07573 | -11.96620 | 15261 | 0.978 | 11.69 | 0.01 | 181 | 18 | 3.3 | PGC959514
WALLABY_J130026-151708 | 195.10945 | -15.28555 | 4920 | 0.345 | 8.74 | 0.01 | 600 | 17 | 4.9 | NGC4877
WALLABY_J130029-181400 | 195.12294 | -18.23359 | 14628 | 0.810 | 15.99 | 0.05 | 98 | 19 | 2.1 |
WALLABY_J130029-133942 | 195.12305 | -13.66192 | 6392 | 0.310 | 16.35 | 0.07 | 76 | 40 | 1.2 |
WALLABY_J130029-133839 | 195.12349 | -13.64420 | 4331 | 0.265 | 12.62 | 0.01 | 158 | 19 | 3.0 | PGC044776
WALLABY_J130032-123039 | 195.13338 | -12.51109 | 6359 | 0.680 | 14.34 | 0.01 | 136 | 17 | 5.3 | PGC951730
WALLABY_J130033-122307 | 195.14067 | -12.38545 | 2500 | 0.750 | 16.43 | 0.13 | 45 | 16 | 5.8 | PGC953585
WALLABY_J130037-143948 | 195.15587 | -14.66346 | 2701 | 0.562 | 10.61 | 0.01 | 150 | 17 | 5.5 | NGC4887
WALLABY_J130043-185429 | 195.18138 | -18.90821 | 10404 | 0.498 | 14.43 | 0.03 | 225 | 17 | 5.1 | PGC862238
WALLABY_J130043-154253 | 195.18234 | -15.71495 | 1383 | 0.000 | 11.74 | 0.02 | 85 | 17 | 4.9 | PGC044812
WALLABY_J130044-142906 | 195.18745 | -14.48505 | 6422 | 0.200 | 14.48 | 0.03 | 181 | 17 | 5.1 | PGC924035
WALLABY_J130047-130944 | 195.19746 | -13.16238 | 18291 | 0.631 | 13.71 | 0.01 | 264 | 18 | 4.1 | PGC941853
WALLABY_J130047-141534 | 195.19971 | -14.25961 | 4596 | 0.880 | 15.48 | 0.05 | 117 | 17 | 4.8 |
WALLABY_J130049-143608 | 195.20488 | -14.60221 | 6500 | 0.550 | 11.60 | 0.01 | 259 | 18 | 4.3 | PGC3098292
WALLABY_J130049-170522 | 195.20738 | -17.08964 | 4826 | 0.485 | 16.45 | 0.03 | 101 | 19 | 2.3 |
WALLABY_J130052-164149 | 195.21719 | -16.69698 | 4286 | 0.919 | 15.21 | 0.04 | 79 | 19 | 2.9 |
WALLABY_J130052-145506 | 195.21899 | -14.91849 | 13859 | 0.200 | 14.99 | 0.04 | 78 | 19 | 3.1 |
WALLABY_J130053-132655 | 195.22302 | -13.44861 | 2551 | 0.531 | 9.37 | 0.01 | 230 | 16 | 6.1 | NGC4897
WALLABY_J130056-135640 | 195.23347 | -13.94450 | 2654 | 0.677 | 9.25 | 0.01 | 277 | 16 | 6.2 | NGC4899
WALLABY_J130057-172247 | 195.23891 | -17.37990 | 4889 | 0.731 | 14.74 | 0.03 | 87 | 18 | 3.3 | PGC884267
Continued in full in MNRAS
Table 4:  N5044-DR3 galaxies with 2 published spectra WALLABY | PGC no | Name | AGC/HIPASS no | Vsys | Width | err | S/N | flux | Vwal | Wwal
---|---|---|---|---|---|---|---|---|---|---
|  |  |  | km s-1 | km s-1 | km s-1 |  | Jykm s-1 | km s-1 | km s-1
J130943-163617 | 45650 | PGC045650 | HIPASSJ1309-16 | 2575 | 340 |  | 5.4 | 27.18 | 2574 | 347
J130943-163617 | 45650 | PGC045650 | HIPASSJ1309-16 | 2576 | 339 | 14 | 8.9 | 7.62 | 2574 | 347
J131234-173225 | 45877 | PGC045877 | AGC530053 shg05 | 2756 | 385 | 19 | 2.2 | 12.68 | 2757 | 389
J131234-173225 | 45877 | PGC045877 | HIPASSJ1312-17 | 2762 | 376 | 13 | 10.0 | 2.48 | 2757 | 389
J132019-123420 | 46535 | NGC5088 | HIPASSJ1320-12 | 1430 | 235 | 16 | 6.6 | 39.67 | 1431 | 240
J132019-123420 | 46535 | NGC5088 | AGC530112 shg05 | 1432 | 242 | 13 | 14.1 | 42.77 | 1431 | 240
J132043-220256 | 46574 | ESO576-040 | AGC029511 shg05 | 2087 | 185 | 12 | 11.6 | 16.20 | 2089 | 191
J132043-220256 | 46574 | ESO576-040 | HIPASSJ1320-22 | 2082 | 179 | 16 | 5.8 | 3.75 | 2089 | 191
J132947-175747 | 47394 | NGC5170 | AGC029724 | 1503 | 524 | 18 | 3.9 | 71.37 | 1503 | 523
J132947-175747 | 47394 | NGC5170 | HIPASSJ1329-17 | 1502 | 528 | 13 | 11.8 | 5.95 | 1503 | 523
J133541-240428 | 47948 | ESO509-074 | AGC029872 shg05 | 2592 | 354 | 18 | 4.1 | 2.45 | 2572 | 322
J133541-240428 | 47948 | ESO509-074 | HIPASSJ1335-24 | 2586 | 345 | 17 | 4.9 | 8.66 | 2572 | 322
J133802-175254 | 48171 | NGC5247 | AGC029924 shg05 | 1356 | 137 | 8 | 53.5 | 57.73 | 1354 | 137
J133802-175254 | 48171 | NGC5247 | HIPASSJ1338-17 | 1355 | 138 | 13 | 32.9 | 56.62 | 1354 | 137
Table 5:  N5044-DR3 galaxies with 1 published spectrum WALLABY | PGC no | Name | AGC/HIPASS no | Vsys | Width | err | S/N | flux | Vwal | Wwal
---|---|---|---|---|---|---|---|---|---|---
|  |  |  | km s-1 | km s-1 | km s-1 |  | Jykm s-1 | km s-1 | km s-1
J125907-121329 | 44549 | PGC044549 | HIPASSJ1259-12 | 1308 | 97 | 13 | 11.0 | 14.13 | 1312 | 80
J125931-140755 | 44610 | NGC4862 | AGC520377 shg05 | 6456 | 143 | 17 | 4.7 | 3.84 | 6451 | 145
J125956-192430 | 44681 | PGC044681 | HIPASSJ1259-19 | 829 | 52 | 16 | 6.3 | 5.03 | 826 | 45
J130026-151708 | 44761 | NGC4877 | HIPASSJ1300-15 | 4933 | 602 | 15 | 7.4 | 16.39 | 4920 | 600
J130053-132655 | 44829 | NGC4897 | HIPASSJ1300-13 | 2555 | 247 | 13 | 12.7 | 29.33 | 2551 | 230
J130056-135640 | 44841 | NGC4899 | HIPASSJ1301-13B | 2653 | 273 | 100 | 34.7 | 21.09 | 2654 | 277
J130059-143042 | 44847 | NGC4902 | HIPASSJ1300-14 | 2631 | 256 | 13 | 12.5 | 27.93 | 2624 | 240
J130107-133053 | 936912 | PGC936912 | HIPASSJ1300-13B | 1308 | 65 | 14 | 8.7 | 7.15 | 1306 | 62
J130213-145817 | 44977 | NGC4924 | HIPASSJ1302-14A | 4856 | 266 | 14 | 9.3 | 8.36 | 4864 | 267
J130213-171416 | 44982 | PGC044982 | HIPASSJ1302-17 | 750 | 117 | 13 | 11.5 | 27.24 | 726 | 39
J130225-174046 | 45006 | PGC045006 | AGC520412 shg05 | 4652 | 480 | 21 | 5.7 | 11.18 | 4649 | 475
J130311-172230 | 45073 | PGC045073 | HIPASSJ1303-17A | 2965 | 66 | 25 | 7.7 | 10.69 | 2963 | 41
J130314-172514 | 45084 | PGC045084 | HIPASSJ1303-17B | 742 | 118 | 13 | 63.1 | 93.27 | 741 | 118
J130815-210002 | 45524 | ESO575-061 | AGC029274 | 1649 | 165 | 17 | 5.0 | 2.94 | 1649 | 168
J130947-101916 | 45652 | PGC045652 | HIPASSJ1309-10 | 1206 | 207 | 16 | 5.8 | 14.02 | 1210 | 196
J131035-214450 | 45721 | ESO576-003 | AGC029327 shg05 | 2959 | 231 | 16 | 6.6 | 11.27 | 2962 | 238
J131305-195830 | 45911 | ESO576-011 | AGC029361 | 2757 | 309 | 11 | 12.4 | 13.23 | 2759 | 306
J131321-185558 | 45935 | ESO576-012 | AGC029366 shg05 | 6148 | 235 | 17 | 4.9 | 3.19 | 6149 | 237
J131330-193244 | 45952 | NGC5022 | AGC029371 | 3001 | 392 | 18 | 4.3 | 8.46 | 3005 | 398
J131334-152553 | 45958 | PGC045958 | HIPASSJ1313-15 | 2503 | 81 | 15 | 7.9 | 12.19 | 2501 | 73
J131702-104612 | 46252 | IC4216 | HIPASSJ1316-10 | 2839 | 257 | 16 | 5.9 | 7.06 | 2838 | 263
J131706-161516 | 46261 | PGC046261 | AGC530085 shg05 | 2631 | 288 | 19 | 2.9 | 8.27 | 2636 | 279
J131739-213708 | 46299 | ESO576-023 | AGC029435 shg05 | 2947 | 188 | 25 | 2.7 | 6.34 | 2933 | 124
J131835-211758 | 46373 | ESO576-026 | AGC029453 | 1953 | 163 | 18 | 3.9 | 2.40 | 1955 | 181
J131920-145037 | 46441 | NGC5073 | AGC530097 shg05 | 2745 | 385 | 15 | 8.0 | 16.07 | 2746 | 405
J131934-124159 | 46473 | NGC5079 | AGC530104 | 2228 | 235 | 16 | 6.6 | 1.92 | 2223 | 249
J132018-214925 | 46525 | NGC5084 | HIPASSJ1320-21 | 1719 | 662 | 100 | 8.7 | 102.72 | 1719 | 655
J132148-131222 | 46664 | NGC5105 | AGC530120 shg05 | 2903 | 219 | 12 | 11.1 | 14.30 | 2903 | 220
J132430-210729 | 46878 | IC4237 | AGC029585 shg05 | 2667 | 325 | 18 | 3.8 | 14.03 | 2607 | 205
J132441-194214 | 46889 | ESO576-050 | AGC029590 | 1969 | 189 | 14 | 8.7 | 17.01 | 1967 | 192
J132500-240035 | 46920 | ESO508-071 | AGC029599 shg05 | 7378 | 315 | 18 | 4.5 | 3.14 | 7388 | 319
J133017-214446 | 47450 | ESO576-072 | AGC029740 | 7314 | 228 | 100 | 5.6 | 2.45 | 7312 | 248
J133058-215044 | 47505 | ESO577-001 | AGC029757 | 7361 | 379 | 100 | 3.4 | 4.35 | 7366 | 371
J133103-150604 | 47514 | PGC047514 | AGC530277 shg05 | 4232 | 300 | 18 | 4.2 | 6.22 | 4231 | 303
J133208-225710 | 47599 | ESO509-045 | AGC029792 | 5047 | 278 | 19 | 2.8 | 3.20 | 5056 | 266
J133209-245132 | 47600 | ESO509-044 | AGC029789 | 7791 | 450 | 100 | 2.8 | 4.09 | 7790 | 439
J133314-160715 | 47717 | PGC047717 | tmc06 | 6342 | 206 | 100 | 3.4 | 2.35 | 6120 | 683
J133933-222957 | 48300 | ESO577-020 | AGC029955 shg05 | 6998 | 249 | 19 | 2.7 | 2.67 | 7000 | 235
J133949-221815 | 48323 | ESO577-022 | AGC029961 | 5760 | 285 | 17 | 4.7 | 2.62 | 5746 | 302
J134002-252831 | 48346 | IC4315 | AGC029965 | 5163 | 322 | 50 | 3.8 | 3.10 | 5134 | 303
shg05 = Springob et al. (2005) |  |  |  |  |
ctf09 = Courtois et al. (2009) |  |  |  |  |
tmc06 = Theureau et al. (2006) |  |  |  |  |

## Acknowledgements

The Australian SKA Pathfinder is part of the Australia Telescope National
Facility (https://ror.org/05qajvd42) which is managed by CSIRO. Operation of
ASKAP is funded by the Australian Government with support from the National
Collaborative Research Infrastructure Strategy. ASKAP uses the resources of
the Pawsey Supercomputing Centre. Establishment of ASKAP, the Murchison Radio-
astronomy Observatory and the Pawsey Supercomputing Centre are initiatives of
the Australian Government, with support from the Government of Western
Australia and the Science and Industry Endowment Fund. We acknowledge the
Wajarri Yamatji as the traditional owners of the Observatory site. WALLABY
acknowledges technical support from the Australian SKA Regional Centre
(AusSRC) and Astronomy Data And Computing Services (ADACS). AD is supported by
a KIAS Individual Grant PG 087201 at the Korea Institute for Advanced Studies.
AB acknowledges support from the Centre National d’Etudes Spatiales (CNES),
France. PEMP acknowledges support from the Dutch Research Council (NWO)
through the Veni grant VI.Veni.222.364. This research was supported partially
by the Australian Government through the Australian Research Council Centre of
Excellence for Dark Matter Particle Physics (CDM, CE200100008).

This publication makes use of data products from the Wide-field Infrared
Survey Explorer, which is a joint project of the University of California Los
Angeles, and the Jet Propulsion Laboratory/California Institute of Technology,
funded by the National Aeronautics and Space Administration. This research
uses services and data provided by the Astro Data Lab at NSF’s National
Optical-Infrared Astronomy Research Laboratory. The Legacy Surveys consist of
three individual and complementary projects: the Dark Energy Camera Legacy
Survey (DECaLS; Proposal ID #2014B-0404; PIs: David Schlegel and Arjun Dey),
the Beijing-Arizona Sky Survey (BASS; NOAO Prop. ID #2015A-0801; PIs: Zhou Xu
and Xiaohui Fan), and the Mayall z-band Legacy Survey (MzLS; Prop. ID
#2016A-0453; PI: Arjun Dey). DECaLS, BASS and MzLS together include data
obtained, respectively, at the Blanco telescope, Cerro Tololo Inter-American
Observatory, NSF’s NOIRLab; the Bok telescope, Steward Observatory, University
of Arizona; and the Mayall telescope, Kitt Peak National Observatory, NOIRLab.
Pipeline processing and analyses of the data were supported by NOIRLab and the
Lawrence Berkeley National Laboratory (LBNL). The Legacy Surveys project is
honored to be permitted to conduct astronomical research on Iolkam Du’ag (Kitt
Peak), a mountain with particular significance to the Tohono O’odham Nation.

NOIRLab is operated by the Association of Universities for Research in
Astronomy (AURA) under a cooperative agreement with the National Science
Foundation. LBNL is managed by the Regents of the University of California
under contract to the U.S. Department of Energy.

This project used data obtained with the Dark Energy Camera (DECam), which was
constructed by the Dark Energy Survey (DES) collaboration. Funding for the DES
Projects has been provided by the U.S. Department of Energy, the U.S. National
Science Foundation, the Ministry of Science and Education of Spain, the
Science and Technology Facilities Council of the United Kingdom, the Higher
Education Funding Council for England, the National Center for Supercomputing
Applications at the University of Illinois at Urbana-Champaign, the Kavli
Institute of Cosmological Physics at the University of Chicago, Center for
Cosmology and Astro-Particle Physics at the Ohio State University, the
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M
University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho
de Amparo, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de
Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de
Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia,
Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the
Collaborating Institutions in the Dark Energy Survey. The Collaborating
Institutions are Argonne National Laboratory, the University of California at
Santa Cruz, the University of Cambridge, Centro de Investigaciones
Energeticas, Medioambientales y Tecnologicas-Madrid, the University of
Chicago, University College London, the DES-Brazil Consortium, the University
of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi
National Accelerator Laboratory, the University of Illinois at Urbana-
Champaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the Institut de
Fisica d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig
Maximilians Universitat Munchen and the associated Excellence Cluster
Universe, the University of Michigan, NSF’s NOIRLab, the University of
Nottingham, the Ohio State University, the University of Pennsylvania, the
University of Portsmouth, SLAC National Accelerator Laboratory, Stanford
University, the University of Sussex, and Texas A&M University.

BASS is a key project of the Telescope Access Program (TAP), which has been
funded by the National Astronomical Observatories of China, the Chinese
Academy of Sciences (the Strategic Priority Research Program The Emergence of
Cosmological Structures Grant # XDB09000000), and the Special Fund for
Astronomy from the Ministry of Finance. The BASS is also supported by the
External Cooperation Program of Chinese Academy of Sciences (Grant #
114A11KYSB20160057), and Chinese National Natural Science Foundation (Grant #
12120101003, # 11433005). We acknowledge the use of the HyperLeda database
(http://leda.univ-lyon1.fr and the Siena Galaxy Atlas. That was made possible
by funding support from the U.S. Department of Energy, Office of Science,
Office of High Energy Physocs under award number DE-SC0020086 and from the
National Science Foundation under grant AST-1616414.

We thank WALLABY team member Matthew Colless for reading drafts of this paper
and Tobias Westmeier for his management of the WALLABY project. We thank the
referee for pointing out some things that needed clarifying.

## Data Availability

When released, 21 cm profiles in this paper will be curated by the CSIRO ASKAP
Science Data Archive. These profiles can be viewed at
https://github.com/jrmould/wallaby-HI-profiles.

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## Appendix

###  A0.1 SoFiA velocity widths

In addition to the velocity widths we have measured and presented in Table 3,
the SoFiA pipeline for WALLABY provides Wm50999This is distinct from w50 in
the WALLABY catalogue., and the relation between the two is shown in Figure
A1. Both are HI profile widths at 50%, but there is a systematic difference
which is mostly unrelated to signal-to-noise. Both velocity widths are from
velocities on the optical convention. A linear fit has a slope of 0.92 and a
$\chi^{2}$ of 1.3. In other words, the scatter is close to that expected on
the grounds of measurement errors, but the non-unity slope is a quantity to be
noted for investigations that require a calibrated TFR. The mean difference
W50 – Wm50 is –7.7 $\pm$ 0.7 km s-1with no significant difference in the mean
between the high and lower SNR data. We use our measured W50s in this paper,
because measurement errors are computed. Not so for Wm50.

The Wm50 measurements are made by interpolating the WALLABY spectrum at 50% of
the peak flux. This is automated. The w50 values on the other hand are
measured by isolating the region of the spectrum where the galaxy flux is by
setting a cursor. Based on the signal to noise a level of smoothing is chosen
(2, 4, 8 pixels), and the smoothed spectrum is then interpolated similarly.
The conversion of w50 to Wmx takes account of the broadening introduced by
this smoothing. For the full WALLABY survey it may be necessary to adopt the
Wm50 approach. But it will be important to include uncertainty calculation in
the process.

Figure A22: Comparison of SoFiA Wm50s with those in Table 3 for the NGC 5044
field. Crosses are for S/N $>$ 3, open circles for S/N $<$ 3\. The figure
below shows the differences, with the higher S/N in green. The red line is a
running mean.

###  A0.2 Alternative axial ratios

In §3.2 we compared IRAF measurements of axial ratios on $g$ band DECaLS
images with kinematic inclinations. The comparison showed considerable
scatter. Other sources of inclinations are worthy of consideration and we show
them in Figure A2. The measurement of WISE total magnitudes also produces
axial ratios and these are shown in red in the figure. They are biased towards
higher inclinations than the kinematic inclinations. We also wrote an ellipse
fitting program on a different principle from that of the IRAF task aiming at
the 25th $g$ magnitude isophote. Minimization of the deviation from an ellipse
with (a, b, & PA) as the parameters of the isophotal pixels yields the solid
black symbols with error bars in Figure A2. The horizontal axis errors derive
from the covariance matrix of the fit. They seem unrealistically small, but,
while some inclined TFR galaxies are well fitted by ellipses in the outer
disk, others are more irregular in their stellar light distribution, a problem
acknowledged in the original TFR paper (Tully & Fisher 1977). These
inclinations are also biased towards higher inclinations, which the IRAF
inclinations (Figure 13) are not.

Figure A23: Alternative sources of disk inclination. Solid black symbols are
from ellipse fitting to $g$ band with experimental software; the red symbols
are from WISE W1 axial ratios; the blue symbols are from resolved WALLABY
hydrogen maps (open, with beam size correction), (solid, without). All these
are plotted against kinematic inclinations by Deg et al. (2022). Pilot survey
phase 1 data have been included in the solid blue category to more fully
populate the graph, and these have error bars to distinguish them.

The SoFiA source finding algorithm also provides estimates of a and b for the
neutral hydrogen. Inclinations from this axial ratio are plotted in blue, the
solid symbols for the raw b/a, the open symbols for the same galaxies after
subtracting 5 pixelsin quadrature to allow for the WALLABY beam size. The raw
values are biased, but the open ones, which are not biased, have more scatter.
The sample with kinematic models is still small and will remain only a subset
of WALLABY TFR galaxies. However, it is possible that bias in the raw hydrogen
axial ratios can be calibrated out, when more data are available. This might
be the path to dispensing with troublesome optical inclinations.

Finally, the stack of galaxies in Figure A2 at 90∘ axial ratio inclinations is
due to galaxies being measured with b/a $<$ 0.2. This choice of minimum axial
ratio should be revised when more data are obtained. For the time being we
note that –8.7 $\log~{}\sin~{}80^{\circ}$ = 0.06 mag, a small correction.

###  A0.3 CosmicFlows4 distances

The positions of WALLABY galaxies within the Cosmic Web can be studied using
the full matter (dark and luminous) density contrast field (usually denoted
$\delta$) reconstructed from the CosmicFlows- 4 Catalogue of peculiar
velocities (Tully et al. 2023, Courtois et al. 2023). This catalogue now uses
the Baryonic TFR (Kourkchi et al. 2022) to calculate distances, and stellar
masses are obtained from multiwavelength photometry. Our WALLABY galaxies have
W1 photometry, although within the decade multiwavelength galaxy photometry
may be supplied by the Rubin Telescope. For the 10,000 CF4 galaxies we have
compared baryonic masses calculated with stellar masses from W1 as in $\S$2.4
with those published in CF4. The result is in Figure A3, after a correction of
0.525 mag to the W1 magnitudes of Kourkchi et al. , which are from a different
source from the W1 total magnitudes used here and in Paper 1. This allows us
to use a baryonic TFR calibration relation from the adjusted CF4 galaxies,
shown in Figure A4. To be incorporated into CosmicFlows4, the distance moduli
obtained with this calibration also needed a 0.15 mag change for the Hubble
constant used in this paper and that calculated from the CF4 database.

Figure A24: Difference in baryonic mass calculated with W1 magnitudes only and
with the multiwavelength photometry of Kourkchi et al. (2022). Figure A25: The
calibration used in $\S$5.3 for the baryonic TFR,
based on the CF4 galaxies of Kourkchi et al. (2022).

###  A0.4 Siena catalogue TFR for the NGC4808 field

The Siena catalogue (Moustakas et al. 2023) has photometry in the $grz$
bandpasses for bright galaxies over half the sky and aspires to complete sky
coverage outside the Galactic plane. These total magnitudes are measured by
exponential disk fitting which also produces axial ratios. We show the TFR in
the NGC 4808 field for $z$ magnitudes and Siena axial ratios in Figure A5. The
normal cut is applied to inclinations, but no S/N cut is made. This is a
promising new resource for the WALLABY project.

Figure A26: The TFR for the NGC4808 field from Siena catalogue $z$ band
photometry. These magnitudes are on the AB system.