J/ApJ/927/64 30yrs of spectroscopic measurements of VMP DLAs (Nunez+, 2022)
Empirical constraints on core-collapse supernova yields using very metal-poor
damped Lyα absorbers.
Nunez E.H., Kirby E.N., Steidel C.C.
<Astrophys. J., 927, 64 (2022)>
=2022ApJ...927...64N 2022ApJ...927...64N
ADC_Keywords: QSOs; Redshifts; Spectra, optical; Abundances; References;
Supernovae
Keywords: Core-collapse supernovae ; Damped Lyman-alpha systems ;
Quasar absorption line spectroscopy ; Population III stars ;
Nucleosynthesis
Abstract:
We place empirical constraints on the yields from zero- and
low-metallicity core-collapse supernovae (CCSNe) using abundances
measured in very metal-poor (VMP; [Fe/H]≤-2) damped Lyα
absorbers (DLAs). For some abundance ratios ([N,Al,S/Fe]), VMP DLAs
constrain the metal yields of the first SNe more reliably than VMP
stars. We compile a large sample of high-S/N VMP DLAs from over 30yr
of literature, most with high-resolution spectral measurements. We
infer the initial-mass-function-averaged CCSNe yield from the median
values from the DLA abundance ratios of C, N, O, Al, Si, S, and Fe
(over Fe and O). We assume that the DLAs are metal-poor enough that
they represent galaxies in their earliest stages of evolution, when
CCSNe are the only nucleosynthetic sources of the metals we analyze.
We compare five sets of zero- and low-metallicity theoretical yields
to the empirical yields derived in this work. We find that the five
models agree with the DLA yields for ratios containing Si and S. Only
one model (HW10; Heger & Woosley 2010ApJ...724..341H 2010ApJ...724..341H) reproduced the
DLA values for N, and one other model (LC18; Limongi & Chieffi
2018ApJS..237...13L 2018ApJS..237...13L) reproduced [N/O]. We found little change in the
theoretical yields with the adoption of an SN explosion landscape
(where certain progenitor masses collapse into black holes,
contributing no yields) onto HW10, but fixing explosion energy to
progenitor mass results in wide disagreements between the predictions
and DLA abundances. We investigate the adoption of a simple,
observationally motivated initial distribution of rotational
velocities for LC18 and find a slight improvement.
Description:
We compiled a large sample (79 total) of very metal-poor (VMP;
[Fe/H]≤-2) damped Lyα absorbers (DLAs) that were available in
the literature. We re-normalized some of the solar abundances the data
sets used to the Asplund+ (2009ARA&A..47..481A 2009ARA&A..47..481A) solar scale from older
scales.
The majority (∼60%) of sources in our sample have high-resolution
spectroscopic measurements. The observations were mainly split between
the High Resolution Echelle Spectrometer (HIRES) on Keck I and the
Ultraviolet and Visual Echelle Spectrograph (UVES) on the Very Large
Telescope (VLT) UT2 at the European Southern Observatory. HIRES
typically covers a spectral range of 4000-8000Å with a resolution
R>30000. UVES has a spectral range of 3000-8000Å between its red
and blue configuration with a spectral resolution of R≥40000.
The other ∼40% of our sample have medium-resolution spectroscopic
measurements. Their spectra were obtained using the Echelle
Spectrometer and Imager (ESI) on Keck II at a resolution of R∼5000
spanning a spectral range of 3900-10900Å.
Additionally, two sources in our sample had spectra obtained by the
Magellan Inamori Kyocera Echelle (MIKE) echelle spectrograph on the
6.5m Magellan Clay telescope at Las Campanas with R=22000-28000
covering a spectral range 3221-7420Å, and the X-shooter
spectrograph on VLT UT2 with R∼8500 covering a spectral range
3000Å-2.5um.
The majority of our sample has appeared in multiple surveys.
See Section 2.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 178 79 Metal summary of very metal-poor (VMP; [Fe/H]≤-2)
damped Lyα absorbers (DLAs)
--------------------------------------------------------------------------------
Description of file:
datafile1.fits.gz is the original table in FITS format downloaded from
the paper.
See also:
J/A+A/370/426 : UVES sp. of APM BR J0307-4945 (Dessauges-Zavadsky+, 2001)
J/A+A/416/1117 : Abundances in the early Galaxy (Cayrel+, 2004)
J/ApJ/649/L61 : SDSS J155810.16-003120.0 abundances (O'Meara+, 2006)
J/ApJS/171/29 : UCSD/Keck Damped Lya Abundance Database (Prochaska+, 2007)
J/ApJ/708/560 : Spectroscopy of UMa II and Coma Ber (Frebel+, 2010)
J/ApJ/724/341 : Nucleosynthesis of massive metal-free stars (Heger+, 2010)
J/ApJ/723/1632 : Abundance spreads in Bootes I and Segue 1 (Norris+, 2010)
J/ApJ/721/1 : Keck ESI observations of Lyα systems (Penprase+, 2010)
J/ApJ/755/89 : Metallicities of damped Lyα systems (Rafelski+, 2012)
J/ApJ/763/61 : Abund. of 7 red giant members of BootesI (Gilmore+, 2013)
J/A+A/556/A141 : ESO-UVES Advanced Data Products (EUADP) (Zafar+, 2013)
J/ApJ/786/74 : EW measurements of 6 Segue 1 red giants (Frebel+, 2014)
J/A+A/562/A146 : Chemical abundances of 8 metal-poor stars (Ishigaki+, 2014)
J/ApJ/797/21 : Carbon-enhanced metal-poor stars (Placco+, 2014)
J/MNRAS/440/2665 : SDSS J021933.13+200830.2 spectroscopy (Roederer+, 2014)
J/MNRAS/452/4326 : Metal-rich damped Lyα systems at z∼2 (Berg+, 2015)
J/ApJ/801/125 : Carbon in red giants in GCs and dSph galaxies (Kirby+, 2015)
J/ApJ/817/41 : Abundances of 4 metal-poor red giants in BooII (Ji+, 2016)
J/AJ/151/82 : The 4 brightest red giants in Ret 2 (Roederer+, 2016)
J/MNRAS/456/4488 : XQ-100 survey neutral gas (Sanchez-Ramirez+, 2016)
J/ApJ/838/44 : Abund. of the brightest member of Tuc III (Hansen+, 2017)
J/ApJ/838/83 : RVels, abundances & membership in TriII (Kirby+, 2017)
J/ApJ/857/74 : Abundances of 7 new member stars in Tucana II (Chiti+, 2018)
J/A+A/611/A76 : DLAS dust-corrected metallicity (De Cia+, 2018)
J/ApJ/857/46 : Modelled vs observed abund. of EMP stars (Ishigaki+, 2018)
J/ApJS/237/13 : Models & yields of massive stars (Limongi+, 2018)
J/ApJ/852/99 : Abund. of 3 metal-poor stars in Hor I (Nagasawa+, 2018)
J/A+A/630/A104 : Disk and halo stars C, O and Fe abundances (Amarsi+, 2019)
J/A+A/622/L4 : Carbon and oxygen in metal-poor halo stars (Amarsi+, 2019)
J/ApJ/870/83 : Abund. in ultra-faint dwarf gal. GruI & TriII (Ji+, 2019)
J/ApJ/882/177 : Abund. of 4 member stars of Tucana III (Marshall+, 2019)
J/ApJ/891/85 : Manganese abund. in GC & dSph galaxies (de los Reyes+, 2020)
J/MNRAS/502/4009 : Sub-damped Lyman α systems in XQ-100 II (Berg+, 2021)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 A13 --- ID Quasar abbreviated designation
15- 39 A25 --- Name Quasar full name (1)
41- 48 F8.6 --- zabs [1.77/5.94] Redshift of the DLA
50- 54 F5.2 cm-2 logNHI [20/21.8] Log of HI column density
56- 59 F4.2 cm-2 e_logNHI [0.02/0.2] logNHI uncertainty
61 A1 --- l_[Fe/H] Upper limit flag on [Fe/H]
63- 67 F5.2 [Sun] [Fe/H] [-3.45/-1.91] Log of Fe/H abundance
69- 73 F5.3 [Sun] e_[Fe/H] [0.001/0.3]? [Fe/H] uncertainty
75 A1 --- f_[C/H] [<x] Limit flag on [C/H] ("x" when no value)
77- 82 F6.3 [Sun] [C/H] [-3.43/-1.51]? Log of C/H abundance
84- 87 F4.2 [Sun] e_[C/H] [0.03/0.2]? [C/H] uncertainty
89 A1 --- f_[N/H] [<x] Limit flag on [N/H] ("x" when no value)
91- 95 F5.2 [Sun] [N/H] [-4.2/-2.04]? Log of N/H abundance
97- 100 F4.2 [Sun] e_[N/H] [0.04/0.15]? [N/H] uncertainty
102 A1 --- f_[O/H] [<x] Limit flag on [O/H] ("x" when no value)
104- 109 F6.3 [Sun] [O/H] [-3.17/-1.45]? Log of O/H abundance
111- 115 F5.3 [Sun] e_[O/H] [0.015/0.2]? [O/H] uncertainty
117 A1 --- f_[Al/H] [<x] Limit flag on [Al/H] ("x" when no value)
119- 124 F6.3 [Sun] [Al/H] [-3.37/-1.52]? Log of Al/H abundance
126- 129 F4.2 [Sun] e_[Al/H] [0.03/0.2]? [Al/H] uncertainty
131 A1 --- f_[Si/H] [<x] Limit flag on [Si/H] ("x" when no value)
133- 138 F6.3 [Sun] [Si/H] [-3.21/-1.35]? Log of Si/H abundance
140- 144 F5.3 [Sun] e_[Si/H] [0.001/0.2]? [Si/H] uncertainty
146 A1 --- f_[S/H] [<x] Limit flag on [S/H] ("x" when no value)
148- 152 F5.2 [Sun] [S/H] [-2.64/-1.21]? Log of S/H abundance
154- 157 F4.2 [Sun] e_[S/H] [0.01/0.17]? [S/H] uncertainty
159- 168 A10 --- Inst Instrument used to obtain spectra/measure
abundance ("ESI", "HIRES", "UVES", "MIKE" or
"XSHOOTER")
170- 178 A9 --- Ref Reference code (2)
--------------------------------------------------------------------------------
Note (1): SDSS J121915.7+102449 in Table 1 of the paper for SDSS1251+4120 is
very likely a misprint for [VV2006] J125125.3+412000; name corrected
at CDS.
Note (2): Reference code as follows:
1 = Lu et al. 1996ApJS..107..475L 1996ApJS..107..475L
2 = Prochaska & Wolfe 1997ApJ...487...73P 1997ApJ...487...73P
3 = Prochaska & Wolfe 1999ApJS..121..369P 1999ApJS..121..369P
4 = Molaro et al. 2000ApJ...541...54M 2000ApJ...541...54M
5 = Prochaska & Wolfe 2000ApJ...533L...5P 2000ApJ...533L...5P
6 = Dessauges-Zavadsky et al. 2001, J/A+A/370/426
7 = Molaro et al. 2001ApJ...549...90M 2001ApJ...549...90M
8 = Prochaska et al. 2001ApJS..137...21P 2001ApJS..137...21P
9 = Prochaska et al. 2001ApJ...552...99P 2001ApJ...552...99P
10 = Prochaska & Wolfe 2002ApJ...566...68P 2002ApJ...566...68P
11 = Dessauges-Zavadsky et al. 2001, J/A+A/370/426
12 = Ledoux et al. 2003MNRAS.346..209L 2003MNRAS.346..209L
13 = Prochaska et al. 2003ApJS..147..227P 2003ApJS..147..227P
14 = Prochaska et al. 2003ApJ...595L...9P 2003ApJ...595L...9P
15 = O'Meara et al. 2006, J/ApJ/649/L61
16 = Noterdaeme et al. 2007A&A...469..425N 2007A&A...469..425N
17 = Prochaska et al. 2007, J/ApJS/171/29
18 = Noterdaeme et al. 2008A&A...481..327N 2008A&A...481..327N
19 = Petitjean et al. 2008A&A...480..349P 2008A&A...480..349P
20 = Pettini et al. 2008MNRAS.385.2011P 2008MNRAS.385.2011P
21 = Ellison et al. 2010MNRAS.406.1435E 2010MNRAS.406.1435E
22 = Penprase et al. 2010, J/ApJ/721/1
23 = Srianand et al. 2010MNRAS.405.1888S 2010MNRAS.405.1888S
24 = Balashev et al. 2011MNRAS.418..357B 2011MNRAS.418..357B
25 = Cooke et al. 2011MNRAS.417.1534C 2011MNRAS.417.1534C
26 = Cooke et al. 2011MNRAS.412.1047C 2011MNRAS.412.1047C
27 = Cooke et al. 2012MNRAS.425..347C 2012MNRAS.425..347C
28 = Cooke & Madau 2014ApJ...791..116C 2014ApJ...791..116C
29 = Dutta et al. 2014MNRAS.440..307D 2014MNRAS.440..307D
30 = Zafar et al. 2014MNRAS.445.2093Z 2014MNRAS.445.2093Z
31 = Cooke et al. 2015ApJ...800...12C 2015ApJ...800...12C
32 = Cooke et al. 2016ApJ...830..148C 2016ApJ...830..148C
33 = Morrison et al. 2016ApJ...830..158M 2016ApJ...830..158M
34 = Cooke et al. 2017MNRAS.467..802C 2017MNRAS.467..802C
35 = D'Odorico et al. 2018ApJ...863L..29D 2018ApJ...863L..29D
36 = Welsh et al. 2019MNRAS.487.3363W 2019MNRAS.487.3363W
37 = Welsh et al. 2020MNRAS.494.1411W 2020MNRAS.494.1411W
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(End) Emmanuelle Perret [CDS] 20-Dec-2023