combustion flame is expected to be extinguished before it reaches the H-rich
envelope, and thus explosive nucleosynthesis would remain confined to the
core. As in SNe Ia, explosive nucleosynthetic yields of SNe I1/2 will be
significantly affected by the details of the explosion mechanism (see e.g.
Mazzali et al., 2007, and references therein). It is also important to note
the presence of high amounts of H from the relatively massive envelope
existing at the moment of the explosion would also be present in the SN I1/2
spectrum, and thus make it more similar to that of type-II SN in this respect.

The relevance of hot bottom burning nucleosynthesis is model dependent. The
primordial 5 and 7 M⊙ stars from Lau et al. (2008) showed a relatively mild
hot bottom burning, leading to ${\rm X_{surf}(^{14}N)/X_{surf}(^{12}C)}\sim$ 5
at the end of thermal pulses, whereas the same models computed with
overshooting led to ${\rm X_{surf}(^{14}N)/X_{surf}(^{12}C)}\sim 100$ at the
end of calculations (Lau et al., 2009). The surface abundances of the
primordial 4 M⊙ model in Figure 9 do not show any effect of hot bottom burning
until after the cessation of thermal pulses. However, when this process
occurs, it develops as a very hot hot bottom burning. The nucleosynthetic
signatures of such extreme hot bottom burning are primarily a large production
of He but also 12,13C, 14N, and even of some O isotopes. Additionally,
although no $s$-process elements are dredged up during the AGB phase of these
stars, they are produced in the intershell (via 22Ne neutron source). The
products processed during pre-supernova evolution could either be expelled in
the SN I1/2 explosion, adding to the ISM inventory of s-process elements, or
destroyed during the explosion itself. Detailed calculations should be
performed in order to obtain the detailed nucleosynthetic yields.

SN I1/2 in binary systems have been suggested as possible candidates to
explain CEMP-$r/s$ stars (item d of section 6) by several authors (Zijlstra,
2004; Wanajo et al., 2006; Abate et al., 2016) but these progenitors present a
number of problems, e.g. population synthesis studies do not reproduce the
observed proportion of CEMP-$s$ to CEMP-$r/s$ stars (Abate et al., 2016). It
should also be noted that many authors consider that the SN I1/2 explosion
would destroy the progenitor (Nomoto, 1987), so the resulting CEMP stars would
not be detected as binaries. However, Hansen et al. (2016b) showed the
existence of single CEMP-s stars and the occurrence of single CEMP-r/s cannot
be discarded.

###  7.3 Nucleosynthesis in EMP stars undergoing ‘normal’ thermally-pulsing
AGB and Super-AGB evolution

Figure 13: Evolution of the surface abundances of some selected isotopes for a
7 M⊙ model with $Z=10^{-5}$ computed with monstar and monsoon (see text for
details).

Intermediate-mass primordial models which implement some overshooting below
the envelope allow for more or less efficient third dredge-up, envelope
pollution and stellar winds (Chieffi et al., 2001; Siess et al., 2002). The
efficiency of the third dredge-up process thus has a strong impact on the
yields and the dependence on the stellar mass was studied by Gil-Pons et al.
(2013) in their $Z=10^{-5}$ models. These authors, who use the search for
neutrality approach to determine the convective boundaries (Frost & Lattanzio,
1996), obtain high values of the dredge-up parameter $\lambda$101010The
$\lambda$ parameter is defined as $\lambda=\frac{\Delta
M_{\mathrm{dredge}}}{\Delta M_{\mathrm{core}}}$, where $\Delta
M_{\mathrm{dredge}}$ is the H-exhausted core mass dredged-up by the convective
envelope after a thermal pulse, and $\Delta M_{\mathrm{core}}$ is the amount
by which the core has grown during the previous interpulse period. for model
stars up to 7 M⊙, for which $\lambda=0.78$. This value decreases with the
stellar mass ($\lambda=0.48$ for the 8 M⊙ model), and becomes very small
($\lambda=0.05$) for the 9 M⊙ model. Together with a thorough analysis of the
evolution, Gil-Pons et al. (2013) presented a limited set of nucleosynthetic
yields for stars between 4 and 9 M⊙, including 1H, 4He, 12C, 14N, 16O, and
Zother, representing all the isotopes beyond 16O.

The nucleosynthetic yields of intermediate-mass and massive-stars were
computed by Chieffi et al. (2001) and Limongi et al. (2000), respectively.
Abia et al. (2001) used these existing yields to assess the contribution of
intermediate-mass and massive stars to the the pollution of the early
intergalactic medium. Campbell & Lattanzio (2008) also presented yields of
primordial and very low metallicity stars in the low- and intermediate-mass
range, although only up to 3 M⊙. Primordial star yields in the intermediate-
mass range are strongly affected by the unknowns in mass-loss rates and
dredge-up efficiency during the thermally-pulsing AGB phase. Therefore, a
detailed study of the effects of different input physics, not only for
primordial compositions but also up to initial metallicity $Z=10^{-5}$, is
badly needed.

Nevertheless, we can attempt to draw some conclusions from the existing
literature. As we may expect from the results for primordial stars of $\rm
M_{ZAMS}\gtrsim$ 3 M⊙ which have experienced efficient envelope pollution, the
models of 3 M⊙$\rm\lesssim M_{ZAMS}\lesssim$ 7 M⊙ by Chieffi et al. (2001) and
Siess et al. (2002) show efficient hot bottom burning. In general models that
experience hot bottom burning display an increase in their surface abundances
of 4He and 14N at the expense of 12C. However, the very high temperature at
which hot bottom burning is operating in massive AGB and Super-AGB stars leads
to a slight production of 12C. This is also seen in the more metal-rich Super-
AGB stars of Siess (2010) that do not experience third dredge-up. Besides,
23Na is processed at the expense of 22Ne, and 26Al from 25Mg. The 7Li produced
during hot bottom burning would be quickly destroyed and thus its contribution
to yields would be negligible (Abia et al. 2001 and Siess et al. 2002).
Depending on the efficiency of the third dredge-up, the surface 12C can be
strongly affected (see e.g. Doherty et al., 2014b).

Siess & Goriely (2003) analysed $s$-process nucleosynthesis in a primordial 3
M⊙ star. They found that the neutrons released from the
$\rm{}^{13}C(\alpha,n)^{16}O$ reaction would be captured by isotopes between C
and Ne. The heavier species synthesized would then act as seeds to form
$s$-process elements. Once transported to the surface by third dredge-up,
these stars are expected to display Pb and Bi enhancements (see also Suda et
al., 2017a). Cruz et al. (2013) also computed and analysed s-process
nucleosynthesis in 1 M⊙ stars between primordial and $Z=10^{-7}$. They
emphasised the effects of input physics uncertainties on their yields.

We now illustrate the detailed nucleosynthesis of $Z=10^{-5}$ models by
showing results computed with monstar and the post-processing nucleosynthesis
program monsoon, e.g. Doherty et al. (2014a). Figure 13 shows a 7 M⊙ model
(Gil-Pons et al. 2018, in preparation). The effects of hot bottom burning (the
average temperature of the base of the convective envelope during the
thermally-pulsing Super-AGB phase is 114$\times 10^{6}\>K$) can be seen in the
increase in 14N, 13C and 17O and, to a lesser extent, of 21Ne and 26Mg,
together with a decrease of 15N. The onset of the Mg-Al chains results in the
depletion of most 24Mg and an increase in 26Al, which at high temperatures
captures a proton to give 27Al (Siess & Arnould, 2008), and subsequently 28Si
(Ventura et al., 2011). Some of the effects of hot bottom burning are
suppressed by efficient third dredge-up, which replenishes 12C after each
pulse. $\alpha-$captures on 12C in the intershell convective region and
subsequent third dredge-up produce surface enhancements in 16O, 20Ne, and 24Mg
while 28Si production is mainly due to proton capture reactions and a leakage
from the Mg-Al chain. It is also important to note the 22Ne enhancement,
because the occurrence of the $\rm{}^{22}Ne(\alpha,n)^{25}Mg$ reaction may be
an important source of neutrons and, consequently, relevant for $s$-process
nucleosynthesis in massive AGB and Super-AGB stars.

It has been reported that stars with $Z_{\mathrm{ZAMS}}\leq 10^{-4}$ and
masses above 8 M⊙ experience high envelope pollution caused by corrosive
second dredge-up (Gil-Pons et al., 2013; Doherty et al., 2014b). The large
amount of 12C dredged-up during this event increases the molecular opacities
in the envelope and then drives stellar winds similar to those of a higher $Z$
object. These low-$Z$ Super-AGB stars also present very efficient hot bottom
burning, but their low third dredge-up efficiency together with the thinness
of the intershell regions hampers the possibility of a strong $s$-enhancement
in models with $\rm M_{ZAMS}\gtrsim$ 8 M⊙. Their nucleosynthesis is similar to
that of their slightly lower mass hot bottom burning counterparts. The yields
of all the models computed by Gil-Pons et al. (2013) and, in particular, for
their 8 and 9 M⊙ models, have [C/Fe] $\geq$ 2\. If this feature is maintained
at the lowest metallicities ($Z<10^{-5}$), 8 to 9 M⊙ stars of the first (few?)
generation(s) would then have the same properties as some CEMP-no stars,
making them potential progenitor candidates. According to the present IMF this
mass range does not account for a significant number of stars, but given that
the primitive IMF might be biased to higher masses, their contribution might
be relevant. These models might also help to explain some NEMP stars,
described in item h of section 6, as polluters of the gas clouds in which they
formed.

Meynet & Maeder (2002) investigated the evolution of rotating $Z=10^{-5}$
models and obtained high 12C and 14N surface enrichments in their
intermediate-mass stars. However these authors only computed a few thermal
pulses and therefore no complete nucleosynthetic yields were provided.

The most massive Super-AGB stars, which experience a dredge-out process, have
been suggested as a site for the formation of neutron-capture elements and, in
particular, for the occurrence of the $i$-process (Petermann et al. 2014,
Doherty et al. 2015, Jones et al. 2016). This intriguing hypothesis is still
to be demonstrated and carefully analysed, probably requiring 3D
hydrodynamical techniques.

The low- and intermediate-mass EMP stars considered in this section are also
likely to have a binary companion. Actually binarity has been a key to some of
the most successful scenarios to interpret EMP stars (see, e.g. Starkenburg et
al. (2014) and references therein). If a star undergoing a dual flash, or
simply third dredge-up of $s$-process elements, is the primary component
(initially the more massive star) of an interacting binary system, then the
$s$-process elements synthetized by the primary can be transferred to its
companion. If such a companion has a mass $\rm M_{ZAMS}$ about 0.8 M⊙ it can
survive to the present day and be detected as a CEMP-$s$ star, as referred to
in items d and e. Note that high amounts of C are expected to be dredged-up,
together with the $s$-process elements. This binary scenario for the formation
of CEMP stars (e.g. Suda et al. 2004) was in agreement with the radial
velocity data of CEMP-$s$ stars, which was consistent with all of them being
members of binary systems (Lucatello et al. 2005, Starkenburg et al. 2014).
However, updated results of radial-velocity monitoring of CEMP stars show that
not all CEMP-s stars are in binary systems (Hansen et al., 2016b), although
the percentage of CEMP-s in binaries is still considerably higher than in
normal metal-poor stars.

###  7.4 Cautionary remarks

One should be cautious when interpreting EMP abundances using nucleosynthetic
yields of model stars. To begin with, if the observed object is a giant, it
may have undergone internal pollution as a consequence of evolutionary
processes. Additionally, even dwarf stars may experience mixing processes such
as thermohaline mixing (Stancliffe et al., 2011), gravitational settling
(Richard et al. 2002, MacDonald et al. 2013), radiative levitation (Matrozis &
Stancliffe, 2016), mixing induced by rotation or gravity waves (e.g. Talon,
2008), or accretion from the ISM (Yoshii 1981, Iben 1983, Komiya et al. 2015).
All these processes may alter surface abundances after accretion from a more
evolved companion star, and must be disentangled if we are to understand the
stellar nucleosynthesis.

The problem of interpreting the abundances of individual EMP stars is
complicated because some of these stars may originate from a second stellar
generation. This second generation probably formed in mini-halos (see e.g.
Schneider et al., 2012; Chiaki et al., 2013; Ji et al., 2015)), as we think
Pop III stars did, in a cloud polluted by gas from a few SN explosions, which
was partially retained and partially ejected from the minihalo. Some of the
ejected gas could have been re-accreted and then mixed with originally
pristine gas and matter from nearby SNe. Therefore nucleosynthetic yield
information should be complemented with chemical evolution models which take
into account mixing and turbulence (Ritter et al., 2015).

##  8 SUMMARY AND DISCUSSION

###  8.1 Summary

The birth, evolution, fate and nucleosynthetic yields of the first generations
of stars remain, in many senses, enigmatic. We have seen that the solution to
this puzzle is hampered by the specific computational problems which plague
the evolution of the most metal-poor stars (such as violent thermonuclear
runaways, thousands of thermal pulses, or unexpected instabilities), by the
high sensitivity of results to the details of very uncertain input physics (in
particular to opacities, mass-loss rates, convection and mixing, as well as
some key nuclear reaction rates), and by the difficulties in obtaining
constraints from observational data.

The occurrence of primordial low- and intermediate-mass stars, strongly
debated during the last few decades, is supported by recent high resolution
3D-hydrodynamical calculations of primordial star formation. In terms of the
final fates of intermediate-mass stars, different authors agree (except for
the precise mass threshold), that primordial to $Z\sim 10^{-7}$ stars of
initial mass $\rm M_{ZAMS}\lesssim$ 4 M⊙ experience efficient mixing episodes
(Campbell & Lattanzio 2008, Lau et al. 2009, Suda & Fujimoto 2010 and
references therein), either prior to or during the first pulses of their
thermally-pulsing AGB phase. These processes enrich the stellar envelopes in
metals, and permit later evolution to take place in a way that is very similar
to that of higher $Z$ stars. Thus we expect these stars to form white dwarfs.
In the low metallicity range considered in this review, the same fate is
expected for stars in the mass range 8 M⊙ $\rm\lesssim M_{ZAMS}\lesssim$ 9.5
M⊙. On the other hand, the fate of $Z\lesssim 10^{-7}$ stars between $\sim$ 4
and $\sim$ 7 M⊙ is more intriguing, and whether they end as white dwarfs or
SNe strongly depends on the choice of input physics. The use of different
algorithms to determine convective boundaries may lead to the occurrence of
SNe I1/2 (Gil-Pons et al., 2008; Lau et al., 2008), whereas the inclusion of
overshooting would probably lead to the formation of white dwarfs (Chieffi et
al., 2001; Siess et al., 2002). We find that the mass range for EC-SNe is
relatively narrow, of the order of $\sim$0.2 M⊙ between $\sim 9.2-9.5$ M⊙ and
$\sim 9.7-9.9$ M⊙ for the $Z=10^{-5}$ and primordial cases, respectively.

The nature, evolution, and fate of models of ancient stars must be tested by
comparing nucleosynthetic yields with observations of the most metal-poor
objects. The sample of metal-poor stars has significantly increased during the
last decade, but the interpretation of the surface abundances remains
difficult because of internal mixing processes, potential pollution by the
ISM, and because the chemodynamical evolution of their parental clouds is not
well understood. Many observational features may be reproduced by rotating
massive stars (Maeder & Meynet, 2015) and supernova models (Umeda & Nomoto
2003, Tominaga et al. 2014) or by low- and intermediate-mass models in binary
stars (Suda et al., 2004). Traditionally, CEMP-no stars were interpreted as
second generation stars formed from a mixture of pristine material and ejecta
from massive Pop III stars, while the CEMP-$s$ stars were thought of as the
low-mass primordial (or second generation) companion of an intermediate-mass
star that went through its thermally-pulsing AGB phase and then polluted its
low-mass partner with $s$-elements. We show in this work that primordial
intermediate-mass model stars might also help to explain some cases of the
heterogeneous CEMP-no group, and that massive star models including rotation
may account for some $s$-process enhancement (Cescutti et al. 2013,
Frischknecht et al. 2016, and Choplin et al. 2017), and thus for the formation
of some CEMP-s stars. The present classification of observations, albeit
useful, might mask the nucleosynthetic contributions of stars over a
continuous mass and metallicity range.

Finally, it is important to note that the relatively restricted sample of
observed EMP stars is not the only limitation. An understanding of the
existing observational results will probably remain incomplete until modelling
the entire evolution of intermediate-mass EMP stars with reasonably precise
input physics is possible.

###  8.2 Present open questions

In spite of the wealth of interesting results obtained during the last
decades, both from the theoretical and the observational point of view, many
questions related to EMP stars remain unanswered.

  * i)

Do low- and intermediate mass stars exist at all $Z$, or is there a critical
metallicity below which they cannot form? If such a limit exists, it is
important to know if its value is closer to 10-8 or to 10-6. Stars born with
the former metallicity behave similarly to primordial objects and, for
instance, might allow the formation of SNe I1/2, whereas the general behaviour
of $Z=10^{-6}$ objects more resembles that of ‘normal’ metallicity stars, at
least in terms of their final fates.

  * ii)

Did SNe I1/2 ever explode? If they have existed there might be interesting
observational consequences. They would synthesise large amounts of Fe-peak
elements, and thus might provide a substantial increase in the injection of
Fe-group elements much earlier than that provided by SN Ia explosions. The
problem is that early Fe should also be significantly produced in primordial
hypernovae, and thus the actual origin of this element in the primitive
Universe will not be easy to disentangle, unless additional isotopes of
intermediate-mass and heavy metals are considered. Stars which are
simultaneously very old and relatively metal-rich might be detected by using
asteroseismology techniques applied to Galactic archeology, as proposed by
Miglio et al. (2013). Additionally, Bergemann et al. (2016) presented a new
method to determine ages of red-giant stars, for [Fe/H] $\leq-2$. However, it
is critical to highlight that the huge uncertainties in models of EMP stars
may considerably complicate age determinations. A fruitful application of
either age-determination method and, eventually, the assessment of the
contribution of SNe I1/2 to the chemical evolution of the Universe should, in
any case, use detailed nucleosynthetic yields of models leading to these
supernovae. In relation to possible descendants of SNI1/2 it is interesting to
consider stars from the Galactic bulge. According to cosmological models (see,
for instance, White & Springel 2000, and Tumlinson 2010) the Bulge should host
the oldest stars in the Galaxy. However, observations show that the average
metallicity of bulge stars is higher than those from the Halo. Besides, metal-
poor stars detected in the Bulge present intriguing peculiarities, such as the
absence of C enhancement, and large $\alpha$-element scatter (Howes et al.,
2014, 2016). The interpretation of these peculiarities will shed light on our
understanding of the oldest stars and, perhaps, on SNI1/2. The latter
explosions might actually appear in the high redshift transient records of new
generation telescopes. However, given the relatively low brightness expected
for SN I1/2, a more promising possibility might be to look for them among the
supernovae discovered in gravitational lenses (Quimby et al. 2013, Kelly et
al. 2015; Goobar et al. 2017), as brightness magnifications of up to
$\times$2000 have been observed (Kelly et al., 2018). While the supernova
brightness could be affected by microlensing due to individual objects in the
lensing galaxy (Dobler & Keeton, 2006), their spectra would be unaffected, and
could become an effective way to classify the observed supernovae.

  * iii)

What are the roles of overshooting, extra-mixing processes, and rotation, in
the evolution of EMP stars? This question is related to item ii, as we have
seen that the inclusion of overshooting may avoid the formation of SNe I1/2.
Additional mixing induced by rotation might lead to effects similar to those
of overshooting.

  * iv)

If low-mass ($\rm M_{ZAMS}\lesssim 0.8$ M⊙) primordial stars ever formed,
could they be unambiguously detected? The possibility that Fe-deprived objects
might remain as such is another matter of debate. Frebel et al. (2009)
performed kinematical analysis on extensive samples of metal-poor stars, and
concluded that ISM pollution was practically negligible. If this is the case,
the absence of detection of Fe-deprived objects would be a direct consequence
of the fact that they do not exist, at least for initial masses $\rm
M_{ZAMS}\lesssim 0.8$ M⊙. Tanaka et al. (2017) and Suzuki (2018) performed
magnetohydrodynamical simulations for stellar winds driven by Alfvén waves,
and also determined that ISM accretion on primordial low-mass stars should be
negligible. On the other hand, Komiya et al. (2015) concluded, on the basis of
chemical evolution studies that accretion from the ISM might lead to
primordial envelope pollution values as high as [Fe/H] $\sim-5$.

  * v)

Could CEMP-no stars form from low- and intermediate mass objects? CEMP-no
stars are traditionally assumed to have formed from a previous generation of
massive stars from which they inherited their chemical peculiarities, but
doubts have been cast on this hypothesis. Considering the continuity of the
[Ba/C] distribution as a function of [Fe/H] in CEMP-$s$ and CEMP-no stars,
Abate et al. (2015b) and Suda et al. (2017a) suggested that CEMP-$s$ and
(some) CEMP-no objects might have a common origin involving binarity.
Observational studies that analysed the binary fraction of different
subclasses of CEMP stars support this hypothesis (Starkenburg et al., 2014;
Hansen et al., 2016a). Similar ideas are discussed in terms of carbon
abundances in CEMP-no stars. Bonifacio et al. (2015) define two groups of CEMP
stars, namely high- and low-carbon band stars. They insist that high-carbon
band stars, consisting of almost all the CEMP-s stars and some CEMP-no stars,
are in binaries. On the other hand, the classification of CEMP stars by Yoon
et al. (2016) leads to a different conclusion. They consider that the carbon
enhancement of CEMP-no stars is intrinsic, and due to the enrichment of their
natal clouds by high-mass progenitor stars.

  * vi)

Could CEMP-$s$ stars be the offspring of massive stars? The standard scenario
for the formation of CEMP-$s$ stars involves a binary. However, recent studies
(Hansen et al., 2016b) revealed the existence of isolated CEMP-s stars. The
fact that massive star models with different rotation rates can reproduce the
observed [Sr/Ba] spread in CEMP stars (Cescutti et al., 2013; Frischknecht et
al., 2016) provides additional support to this scenario which was recently re-
investigated by Choplin et al. (2017).

###  8.3 Future topics of research

Below we discuss some bottlenecks in our understanding of EMP stars, and also
areas that may provide promising avenues for further research.

  * i)

As is always the case, a better understanding of convection and, in
particular, of convective boundaries, is a significant barrier to more
reliable models. When dealing with stars at the most metal-poor regimes we
have little insights into the how to model convection and its borders. We are
forced to extrapolate or adapt the existing observational and theoretical
information from higher $Z$\- objects, and we must be aware of the possibility
(and high probability) of introducing substantial errors. In spite of these
uncertainties there is a reasonable consensus on the evolution and fates of
the less massive intermediate-mass objects at the lowest $Z$. On the other
hand our knowledge of the final fates of the most metal poor stars ($Z\lesssim
10^{-7}$) of masses between $\sim$ 4 M⊙ and 8 M⊙ is very poorly constrained.
Work is proceeding to improve the physics on the treatment of convection and
convective boundaries beyond the MLT (see e.g. Arnett et al., 2015; Campbell
et al., 2016; Arnett & Moravveji, 2017).

  * ii)

A better understanding of low-temperature opacities and mass-loss rates is
crucial. Recent improvements in opacity tables by Lederer & Aringer (2009) and
Marigo & Aringer (2009) have been implemented in models and their important
consequences in terms of stellar wind enhancements have been reported, for
instance, in Constantino et al. (2014). The effects of dust in low-temperature
opacities might be even more significant (Tashibu et al., 2017). Intermediate-
mass models with compositions from primordial to $Z=10^{-7}$ should be
constructed considering these effects, although the high effective temperature
and almost pristine composition of these stars suggest that their evolution
would be less sensitive to these changes.

  * iii)

The phenomenon of thermal pulses ceasing and then re-starting is not
understood, and is ripe for investigation. We need a consistent set of
calculations with different ‘reasonable’ input physics for these models. The
envelope pollution and increase of mass-loss rates associated with the re-
onset of thermal pulses might eventually hamper the formation of SNe I1/2.

  * iv)

Many CEMP-s, and some CEMP-no stars have a binary companion. Addressing the
problem of their evolution, including mass transfer via wind accretion, should
also be a priority (Bisterzo et al. 2011 and Abate et al. 2015a ).

  * v)

Improvement in our knowledge of the former issues will help us to obtain
better evolutionary models and nucleosynthetic yields, including full
n-capture nucleosynthesis. Ultimately we want to combine these yields with
sophisticated chemical evolution models, in order to get a more realistic
approach to the interpretation of EMP abundances (e.g. Ritter et al. 2015,
Hirai et al. 2018). Dwarf galaxies seem to be promising tools because their
formation history is not as complicated as that of the Milky Way.

The current revolution in stellar spectroscopy is changing the landscape. The
development of very large telescopes, enormous surveys and machine learning is
driving this revolution. These will allow us to get further information from
medium resolution data, so that dwarf galaxies can be analysed (Kirby et al.,
2015). Komiya et al. (2016) proposed that Pop III stars freed from their
massive companions and undergoing a SN explosion could be detected by large-
scale giant surveys in the outskirts of the Milky Way. Magg et al. (2018) also
calculated the probability of finding Pop III survivors. Their results were
compatible with the absence of detection in the Milky Way, but yielded
somewhat more promising results for its dwarf satellites. However only giants
are expected to be observed in them, which reduces the detection probability.

The faintness of ancient stars is indeed a challenge for their detection.
However, if the end of the lives of some of these stars is marked by SN I1/2
explosions, their luminosity might allow detection with new generation
telescopes such as the James Webb Space Telescope (see de Souza et al. 2014,
and references therein). Detecting and identifying SN I1/2 explosions would
provide us with key information about the primordial IMF and the evolution of
the most ancient stars.

###### Acknowledgements.

The authors thank George Angelou, Takuma Suda, and the anonymous referees for
their useful comments. This work was supported by Spanish MINECO grant
AYA2015-71091-P. This work was supported in part by the National Science
Foundation under Grant No. PHY-1430152 (JINA Center for the Evolution of the
Elements). CD acknowledges support from the Lendulet-2014 Programme of the
Hungarian Academy of Sciences. SWC acknowledges federal funding from the
Australian Research Council though the Future Fellowship grant entitled “Where
are the Convective Boundaries in Stars?” (FT160100046)

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