J/MNRAS/507/4102 Abundances of metal-poor stars from SkyMapper (Yong+, 2021)
High-resolution spectroscopic follow-up of the most metal-poor candidates from
SkyMapper DR1.1.
Yong D., Da Costa G.S., Bessell M.S., Chiti A., Frebel A., Gao X., Lind K.,
Mackey A.D., Marino A.F., Murphy S.J., Nordlander T., Asplund M.,
Casey A.R., Kobayashi C., Norris J.E., Schmidt B.P.
<Mon. Not. R. Astron. Soc. 507, 4102-4119 (2021)>
=2021MNRAS.507.4102Y 2021MNRAS.507.4102Y (SIMBAD/NED BibCode)
ADC_Keywords: Stars, metal-deficient ; Stars, carbon ; Space observations ;
Optical ; Photometry ; Radial velocities ; Spectroscopy ;
Equivalent widths ; Effective temperatures ; Models, atmosphere ;
Abundances ; Abundances, [Fe/H]
Keywords: stars: abundances - stars: Population II -
Galaxy: abundances - early universe
Abstract:
We present chemical abundances for 21 elements (from Li to Eu) in 150
metal-poor Galactic stars spanning -4.1<[Fe/H]←2.1. The targets
were selected from the SkyMapper survey and include 90 objects with
[Fe/H]≤-3 of which some 15 have [Fe/H]≤-3.5. When combining the
sample with our previous studies, we find that the metallicity
distribution function has a power-law slope of
Δ(log N)/Δ[Fe/H] = 1.51 ± 0.01 dex per dex over the range
-4≤[Fe/H]≤-3. With only seven carbon-enhanced metal-poor stars
in the sample, we again find that the selection of metal-poor stars
based on SkyMapper filters is biased against highly carbon-rich stars
for [Fe/H]>-3.5. Of the 20 objects for which we could measure
nitrogen, 11 are nitrogen-enhanced metal-poor (NEMP) stars. Within our
sample, the high NEMP fraction (55 per cent ± 21 per cent) is
compatible with the upper range of predicted values (between 12 per
cent and 35 per cent). The chemical abundance ratios [X/Fe] versus
[Fe/H] exhibit similar trends to previous studies of metal-poor stars
and Galactic chemical evolution models. We report the discovery of
nine new r-I stars, four new r-II stars, one of which is the most
metal-poor known, nine low-α stars with [α]/Fe]≤0.15
as well as one unusual star with [Zn/Fe] = +1.4 and [Sr/Fe] = +1.2 but
with normal [Ba/Fe]. Finally, we combine our sample with literature
data to provide the most extensive view of the early chemical
enrichment of the Milky Way Galaxy.
Description:
We present the high-resolution spectroscopic analysis for a sample of
150 stars selected from SkyMapper photometry that have been vetted
using intermediate-resolution spectroscopy via spectrographs like
WiFeS, MIKE, HIRES, FEROS. We further proceed to data extraction with
their respectives data reduction pipelines (see section 2 Selection,
Observations, and Data Reduction).
Here, the table1.dat shows the programme stars and observing details.
As first results, the table2.dat exhibits the list of optical lines
observed for each stars, the linked ionized species and the measured
equivalent width used to computed element abundances.
Secondly, as explained in the section 3 Analysis, we use model
atmospheres NEWODF grid of ATLAS9 models and LTE stellar line analysis
programme MOOG in order to fit observed and synthetic spectra which
leads us to element abundances values. The table3.dat resume the model
atmosphere parameters computed for each program stars. Hereafter, the
table5.dat expose the calculated carbon abundances, the table7.dat and
table8.dat reveal the chemical abundances of all found elements for
each stars. To complete the three last tables, the table9.dat resumes
details on total abundance errors.
Finally, the table sup.dat summarizes the stellar parameters, stars
metal-deficient classfications and all the chemical abundances
precisely computed for the 150 metal-poor Galactic stars of our study.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 52 166 Program stars and observing details
table2.dat 947 191 *Line list and equivalent width measurements
table3.dat 66 166 Model atmosphere parameters
table5.dat 41 152 Carbon abundances and the corrections for
evolutionary status
table7.dat 56 2432 Chemical abundances for the program stars
table8.dat 48 111 Chemical abundances for Zn, Y, Zr and Eu
table9.dat 68 2584 Abundance errors from uncertainties in
atmospheric parameters
sup.dat 177 150 Stellar parameters and chemical abundances for
the program metal-poor Galactic stars
--------------------------------------------------------------------------------
Note on table2.dat: Star names are abbreviated to the first four digits in RA
and DEC, e.g., from SMSS J001604.23-024105.0 to 0016-0241. EW means Equivalent
Width.
--------------------------------------------------------------------------------
See also:
J/ApJ/762/25 : The most metal-poor stars in HES and SDSS. I. (Norris+, 2013)
J/ApJ/655/492 : Equivalent widths of 26 metal-poor stars (Aoki+, 2007)
J/ApJ/797/21 : Carbon-enhanced metal-poor stars (Placco+, 2014)
II/358 : SkyMapper Southern Sky Survey. DR1.1 (Wolf+, 2018)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- SMSS Star's name identifier (ID) (G1)
21 A1 --- Tel [F/K/M] Telescope chosen for the
obsvervations (Telescope) (G2)
23- 27 F5.2 mag gmag Apparent magnitude in g-band
from SkyMapper DR1.1 (g)
29- 31 I3 --- SNR Signal-to-noise ratio per pixel near
4500 Angstrom (S/R)
33- 45 F13.5 d JD Julian date of the observation (JD) (1)
47- 52 F6.1 km/s RV Heliocentric radial velocity (RV) (2)
-------------------------------------------------------------------------------
Note (1): The observations occured between the January 17, 2017 and the May 4,
2018.
Note (2): Radial velocities were measured by comparing the observed and
predicted wavelengths of the lines for which equivalent widths were
measured.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 0.1nm Lambda Wavelength of the line (Wavelength)
9- 12 F4.1 --- Ion Species identifier (Species) (1)
14- 17 F4.2 eV LEP Lower excitation potential (LEP)
19- 23 F5.2 --- log(gf) The logarithm of oscillator strength (loggf)
25- 29 F5.1 10-4nm EW0016-0241 ?=- EW for the star 0016-0241 (EW0016-0241)
31- 35 F5.1 10-4nm EW0054-8441 ?=- EW for the star 0054-8441 (EW0054-8441)
37- 41 F5.1 10-4nm EW0111-4950 ?=- EW for the star 0111-4950 (EW0111-4950)
43- 47 F5.1 10-4nm EW0200-4657 ?=- EW for the star 0200-4657 (EW0200-4657)
49- 53 F5.1 10-4nm EW0242-4703 ?=- EW for the star 0242-4703 (EW0242-4703)
55- 59 F5.1 10-4nm EW0302-2814 ?=- EW for the star 0302-2814 (EW0302-2814)
61- 65 F5.1 10-4nm EW0302-2843 ?=- EW for the star 0302-2843 (EW0302-2843)
67- 71 F5.1 10-4nm EW0304-3406 ?=- EW for the star 0304-3406 (EW0304-3406)
73- 77 F5.1 10-4nm EW0306-7501 ?=- EW for the star 0306-7501 (EW0306-7501)
79- 83 F5.1 10-4nm EW0307-6100 ?=- EW for the star 0307-6100 (EW0307-6100)
85- 89 F5.1 10-4nm EW0308-7001 ?=- EW for the star 0308-7001 (EW0308-7001)
91- 95 F5.1 10-4nm EW0309-5440 ?=- EW for the star 0309-5440 (EW0309-5440)
97-101 F5.1 10-4nm EW0317-3740 ?=- EW for the star 0317-3740 (EW0317-3740)
103-107 F5.1 10-4nm EW0345-7247 ?=- EW for the star 0345-7247 (EW0345-7247)
109-113 F5.1 10-4nm EW0347-7513 ?=- EW for the star 0347-7513 (EW0347-7513)
115-119 F5.1 10-4nm EW0435-4704 ?=- EW for the star 0435-4704 (EW0435-4704)
121-125 F5.1 10-4nm EW0438-8319 ?=- EW for the star 0438-8319 (EW0438-8319)
127-131 F5.1 10-4nm EW0441-4848 ?=- EW for the star 0441-4848 (EW0441-4848)
133-137 F5.1 10-4nm EW0502-6429 ?=- EW for the star 0502-6429 (EW0502-6429)
139-143 F5.1 10-4nm EW0517-4253 ?=- EW for the star 0517-4253 (EW0517-4253)
145-149 F5.1 10-4nm EW0523-6218 ?=- EW for the star 0523-6218 (EW0523-6218)
151-155 F5.1 10-4nm EW0537-2442a ?=- EW for the star 0537-2442 (EW0537-2442)
157-161 F5.1 10-4nm EW0537-2442b ?=- EW for the star 0537-2442 (EW0537-2442)
163-167 F5.1 10-4nm EW0546-4714 ?=- EW for the star 0546-4714 (EW0546-4714)
169-173 F5.1 10-4nm EW0549-5946 ?=- EW for the star 0549-5946 (EW0549-5946)
175-179 F5.1 10-4nm EW0549-4539 ?=- EW for the star 0549-4539 (EW0549-4539)
181-185 F5.1 10-4nm EW0622-6757 ?=- EW for the star 0622-6757 (EW0622-6757)
187-191 F5.1 10-4nm EW0624-6230 ?=- EW for the star 0624-6230 (EW0624-6230)
193-197 F5.1 10-4nm EW0636-5516 ?=- EW for the star 0636-5516 (EW0636-5516)
199-203 F5.1 10-4nm EW0721-8357 ?=- EW for the star 0721-8357 (EW0721-8357)
205-209 F5.1 10-4nm EW0743-6127 ?=- EW for the star 0743-6127 (EW0743-6127)
211-215 F5.1 10-4nm EW0748-6201 ?=- EW for the star 0748-6201 (EW0748-6201)
217-221 F5.1 10-4nm EW0811-0542 ?=- EW for the star 0811-0542 (EW0811-0542)
223-227 F5.1 10-4nm EW0816-0559 ?=- EW for the star 0816-0559 (EW0816-0559)
229-233 F5.1 10-4nm EW0823-1150 ?=- EW for the star 0823-1150 (EW0823-1150)
235-239 F5.1 10-4nm EW0830-7349 ?=- EW for the star 0830-7349 (EW0830-7349)
241-245 F5.1 10-4nm EW0843-1415 ?=- EW for the star 0843-1415 (EW0843-1415)
247-251 F5.1 10-4nm EW0844-2643 ?=- EW for the star 0844-2643 (EW0844-2643)
253-257 F5.1 10-4nm EW0852-7612 ?=- EW for the star 0852-7612 (EW0852-7612)
259-263 F5.1 10-4nm EW0855-2346 ?=- EW for the star 0855-2346 (EW0855-2346)
265-269 F5.1 10-4nm EW0901-6210 ?=- EW for the star 0901-6210 (EW0901-6210)
271-275 F5.1 10-4nm EW0910-1444 ?=- EW for the star 0910-1444 (EW0910-1444)
277-281 F5.1 10-4nm EW0911-2646 ?=- EW for the star 0911-2646 (EW0911-2646)
283-287 F5.1 10-4nm EW0922-7125 ?=- EW for the star 0922-7125 (EW0922-7125)
289-293 F5.1 10-4nm EW0923-2038 ?=- EW for the star 0923-2038 (EW0923-2038)
295-299 F5.1 10-4nm EW0930-2357 ?=- EW for the star 0930-2357 (EW0930-2357)
301-305 F5.1 10-4nm EW0935-7155 ?=- EW for the star 0935-7155 (EW0935-7155)
307-311 F5.1 10-4nm EW0952-1857 ?=- EW for the star 0952-1857 (EW0952-1857)
313-317 F5.1 10-4nm EW0952-0855 ?=- EW for the star 0952-0855 (EW0952-0855)
319-323 F5.1 10-4nm EW0954-0021a ?=- EW for the star 0954-0021 (EW0954-0021)
325-329 F5.1 10-4nm EW0954-0021b ?=- EW for the star 0954-0021 (EW0954-0021)
331-335 F5.1 10-4nm EW0955-1904 ?=- EW for the star 0955-1904 (EW0955-1904)
337-341 F5.1 10-4nm EW0958-3227 ?=- EW for the star 0958-3227 (EW0958-3227)
343-347 F5.1 10-4nm EW1013-3720 ?=- EW for the star 1013-3720 (EW1013-3720)
349-353 F5.1 10-4nm EW1020-4810 ?=- EW for the star 1020-4810 (EW1020-4810)
355-359 F5.1 10-4nm EW1024-0828 ?=- EW for the star 1024-0828 (EW1024-0828)
361-365 F5.1 10-4nm EW1027-4111 ?=- EW for the star 1027-4111 (EW1027-4111)
367-371 F5.1 10-4nm EW1032-1315 ?=- EW for the star 1032-1315 (EW1032-1315)
373-377 F5.1 10-4nm EW1038-2848 ?=- EW for the star 1038-2848 (EW1038-2848)
379-383 F5.1 10-4nm EW1055-2155 ?=- EW for the star 1055-2155 (EW1055-2155)
385-389 F5.1 10-4nm EW1109+0754 ?=- EW for the star 1109+0754 (EW1109+0754)
391-395 F5.1 10-4nm EW1112-2212 ?=- EW for the star 1112-2212 (EW1112-2212)
397-401 F5.1 10-4nm EW1128-0646 ?=- EW for the star 1128-0646 (EW1128-0646)
403-407 F5.1 10-4nm EW1135+0228 ?=- EW for the star 1135+0228 (EW1135+0228)
409-413 F5.1 10-4nm EW1159-2610 ?=- EW for the star 1159-2610 (EW1159-2610)
415-419 F5.1 10-4nm EW1202-4009 ?=- EW for the star 1202-4009 (EW1202-4009)
421-425 F5.1 10-4nm EW1205-2959 ?=- EW for the star 1205-2959 (EW1205-2959)
427-431 F5.1 10-4nm EW1206-2914 ?=- EW for the star 1206-2914 (EW1206-2914)
433-437 F5.1 10-4nm EW1216-2812 ?=- EW for the star 1216-2812 (EW1216-2812)
439-443 F5.1 10-4nm EW1217-2721 ?=- EW for the star 1217-2721 (EW1217-2721)
445-449 F5.1 10-4nm EW1218-1610 ?=- EW for the star 1218-1610 (EW1218-1610)
451-455 F5.1 10-4nm EW1222-2521 ?=- EW for the star 1222-2521 (EW1222-2521)
457-461 F5.1 10-4nm EW1236-3435 ?=- EW for the star 1236-3435 (EW1236-3435)
463-467 F5.1 10-4nm EW1251-4216 ?=- EW for the star 1251-4216 (EW1251-4216)
469-473 F5.1 10-4nm EW1251-4243 ?=- EW for the star 1251-4243 (EW1251-4243)
475-479 F5.1 10-4nm EW1257-1054 ?=- EW for the star 1257-1054 (EW1257-1054)
481-485 F5.1 10-4nm EW1333-4654 ?=- EW for the star 1333-4654 (EW1333-4654)
487-491 F5.1 10-4nm EW1344-2357 ?=- EW for the star 1344-2357 (EW1344-2357)
493-497 F5.1 10-4nm EW1355-3750 ?=- EW for the star 1355-3750 (EW1355-3750)
499-503 F5.1 10-4nm EW1435-4203 ?=- EW for the star 1435-4203 (EW1435-4203)
505-509 F5.1 10-4nm EW1435-4719 ?=- EW for the star 1435-4719 (EW1435-4719)
511-515 F5.1 10-4nm EW1436-3631 ?=- EW for the star 1436-3631 (EW1436-3631)
517-521 F5.1 10-4nm EW1447-1955 ?=- EW for the star 1447-1955 (EW1447-1955)
523-527 F5.1 10-4nm EW1447-3308 ?=- EW for the star 1447-3308 (EW1447-3308)
529-533 F5.1 10-4nm EW1455-3405 ?=- EW for the star 1455-3405 (EW1455-3405)
535-539 F5.1 10-4nm EW1457-2613 ?=- EW for the star 1457-2613 (EW1457-2613)
541-545 F5.1 10-4nm EW1459-0916 ?=- EW for the star 1459-0916 (EW1459-0916)
547-551 F5.1 10-4nm EW1510-3956 ?=- EW for the star 1510-3956 (EW1510-3956)
553-557 F5.1 10-4nm EW1510-7939 ?=- EW for the star 1510-7939 (EW1510-7939)
559-563 F5.1 10-4nm EW1523-2225 ?=- EW for the star 1523-2225 (EW1523-2225)
565-569 F5.1 10-4nm EW1536-0131 ?=- EW for the star 1536-0131 (EW1536-0131)
571-575 F5.1 10-4nm EW1543-3000 ?=- EW for the star 1543-3000 (EW1543-3000)
577-581 F5.1 10-4nm EW1543-8318 ?=- EW for the star 1543-8318 (EW1543-8318)
583-587 F5.1 10-4nm EW1545-1020 ?=- EW for the star 1545-1020 (EW1545-1020)
589-593 F5.1 10-4nm EW1546-0810 ?=- EW for the star 1546-0810 (EW1546-0810)
595-599 F5.1 10-4nm EW1557-2939 ?=- EW for the star 1557-2939 (EW1557-2939)
601-605 F5.1 10-4nm EW1606-2530 ?=- EW for the star 1606-2530 (EW1606-2530)
607-611 F5.1 10-4nm EW1625-7629 ?=- EW for the star 1625-7629 (EW1625-7629)
613-617 F5.1 10-4nm EW1630-7156 ?=- EW for the star 1630-7156 (EW1630-7156)
619-623 F5.1 10-4nm EW1638-7943 ?=- EW for the star 1638-7943 (EW1638-7943)
625-629 F5.1 10-4nm EW1647-0011 ?=- EW for the star 1647-0011 (EW1647-0011)
631-635 F5.1 10-4nm EW1647-6519 ?=- EW for the star 1647-6519 (EW1647-6519)
637-641 F5.1 10-4nm EW1652-2712 ?=- EW for the star 1652-2712 (EW1652-2712)
643-647 F5.1 10-4nm EW1655-6641 ?=- EW for the star 1655-6641 (EW1655-6641)
649-653 F5.1 10-4nm EW1655-7255 ?=- EW for the star 1655-7255 (EW1655-7255)
655-659 F5.1 10-4nm EW1701-6511 ?=- EW for the star 1701-6511 (EW1701-6511)
661-665 F5.1 10-4nm EW1703-6709 ?=- EW for the star 1703-6709 (EW1703-6709)
667-671 F5.1 10-4nm EW1712-5848 ?=- EW for the star 1712-5848 (EW1712-5848)
673-677 F5.1 10-4nm EW1723-6023 ?=- EW for the star 1723-6023 (EW1723-6023)
679-683 F5.1 10-4nm EW1726-5906 ?=- EW for the star 1726-5906 (EW1726-5906)
685-689 F5.1 10-4nm EW1726-5759 ?=- EW for the star 1726-5759 (EW1726-5759)
691-695 F5.1 10-4nm EW1730-5329 ?=- EW for the star 1730-5329 (EW1730-5329)
697-701 F5.1 10-4nm EW1747-5713 ?=- EW for the star 1747-5713 (EW1747-5713)
703-707 F5.1 10-4nm EW1753-7035 ?=- EW for the star 1753-7035 (EW1753-7035)
709-713 F5.1 10-4nm EW1801-7327 ?=- EW for the star 1801-7327 (EW1801-7327)
715-719 F5.1 10-4nm EW1812-4631 ?=- EW for the star 1812-4631 (EW1812-4631)
721-725 F5.1 10-4nm EW1827-3419 ?=- EW for the star 1827-3419 (EW1827-3419)
727-731 F5.1 10-4nm EW1828-3540 ?=- EW for the star 1828-3540 (EW1828-3540)
733-737 F5.1 10-4nm EW1831-4822 ?=- EW for the star 1831-4822 (EW1831-4822)
739-743 F5.1 10-4nm EW1833-6450 ?=- EW for the star 1833-6450 (EW1833-6450)
745-749 F5.1 10-4nm EW1848-5534 ?=- EW for the star 1848-5534 (EW1848-5534)
751-755 F5.1 10-4nm EW1848-5506 ?=- EW for the star 1848-5506 (EW1848-5506)
757-761 F5.1 10-4nm EW1853-5554 ?=- EW for the star 1853-5554 (EW1853-5554)
763-767 F5.1 10-4nm EW1856-4217 ?=- EW for the star 1856-4217 (EW1856-4217)
769-773 F5.1 10-4nm EW1856-5638 ?=- EW for the star 1856-5638 (EW1856-5638)
775-779 F5.1 10-4nm EW1857-4933 ?=- EW for the star 1857-4933 (EW1857-4933)
781-785 F5.1 10-4nm EW1904-6026 ?=- EW for the star 1904-6026 (EW1904-6026)
787-791 F5.1 10-4nm EW1905-5818 ?=- EW for the star 1905-5818 (EW1905-5818)
793-797 F5.1 10-4nm EW1905-4547 ?=- EW for the star 1905-4547 (EW1905-4547)
799-803 F5.1 10-4nm EW1908-4016 ?=- EW for the star 1908-4016 (EW1908-4016)
805-809 F5.1 10-4nm EW1936-3546 ?=- EW for the star 1936-3546 (EW1936-3546)
811-815 F5.1 10-4nm EW1945-2325 ?=- EW for the star 1945-2325 (EW1945-2325)
817-821 F5.1 10-4nm EW2001-1028 ?=- EW for the star 2001-1028 (EW2001-1028)
823-827 F5.1 10-4nm EW2003-1142 ?=- EW for the star 2003-1142 (EW2003-1142)
829-833 F5.1 10-4nm EW2026-0047 ?=- EW for the star 2026-0047 (EW2026-0047)
835-839 F5.1 10-4nm EW2029-4002 ?=- EW for the star 2029-4002 (EW2029-4002)
841-845 F5.1 10-4nm EW2034-2951 ?=- EW for the star 2034-2951 (EW2034-2951)
847-851 F5.1 10-4nm EW2050-6613 ?=- EW for the star 2050-6613 (EW2050-6613)
853-857 F5.1 10-4nm EW2109-3635 ?=- EW for the star 2109-3635 (EW2109-3635)
859-863 F5.1 10-4nm EW2117-4045 ?=- EW for the star 2117-4045 (EW2117-4045)
865-869 F5.1 10-4nm EW2121-6117 ?=- EW for the star 2121-6117 (EW2121-6117)
871-875 F5.1 10-4nm EW2128-6113 ?=- EW for the star 2128-6113 (EW2128-6113)
877-881 F5.1 10-4nm EW2134-6224 ?=- EW for the star 2134-6224 (EW2134-6224)
883-887 F5.1 10-4nm EW2146-3125 ?=- EW for the star 2146-3125 (EW2146-3125)
889-893 F5.1 10-4nm EW2147-0815 ?=- EW for the star 2147-0815 (EW2147-0815)
895-899 F5.1 10-4nm EW2151-2025 ?=- EW for the star 2151-2025 (EW2151-2025)
901-905 F5.1 10-4nm EW2158-2029 ?=- EW for the star 2158-2029 (EW2158-2029)
907-911 F5.1 10-4nm EW2222-3416 ?=- EW for the star 2222-3416 (EW2222-3416)
913-917 F5.1 10-4nm EW2223-4824 ?=- EW for the star 2223-4824 (EW2223-4824)
919-923 F5.1 10-4nm EW2241-0646 ?=- EW for the star 2241-0646 (EW2241-0646)
925-929 F5.1 10-4nm EW2305-2138 ?=- EW for the star 2305-2138 (EW2305-2138)
931-935 F5.1 10-4nm EW2307-6937 ?=- EW for the star 2307-6937 (EW2307-6937)
937-941 F5.1 10-4nm EW2321-1605 ?=- EW for the star 2321-1605 (EW2321-1605)
943-947 F5.1 10-4nm EW2348-5148 ?=- EW for the star 2348-5148 (EW2348-5148)
--------------------------------------------------------------------------------
Note (1): As from encoded in Norris et al. (2013ApJ...762...25N 2013ApJ...762...25N,
Cat. J/ApJ/762/25) , ionized species identifier are made as follows:
11.0 = NaI which has 2 associed wavelength lines
12.0 = MgI which has 7 associed wavelength lines
13.0 = AlI which has 2 associed wavelength lines
14.0 = SiI which has 1 associed wavelength lines
20.0 = CaI which has 10 associed wavelength lines
21.1 = ScII which has 2 associed wavelength lines
22.0 = TiI which has 6 associed wavelength lines
22.1 = TiII which has 21 associed wavelength lines
24.0 = CrI which has 5 associed wavelength lines
25.0 = MnI which has 3 associed wavelength lines
26.0 = FeI which has 112 associed wavelength lines
26.1 = FeII which has 7 associed wavelength lines
27.0 = CoI which has 4 associed wavelength lines
28.0 = NiI which has 3 associed wavelength lines
38.1 = SrII which has 2 associed wavelength lines
56.1 = BaII which has 4 associed wavelength lines
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- SMSS Star's name identifier (ID) (G1)
21 A1 --- n_SMSS [*] When SNR < 10 (n_ID) (1)
23 A1 --- Tel [F/K/M] Telescope chosen for the
observations (Telescope) (G2)
25- 28 I4 K Teff Effective temperature (Teff)
30- 33 F4.2 [cm/s2] logg Surface gravity (logg)
35- 37 F3.1 km/s vt Microturbulence velocity (Ξt)
39- 42 F4.1 [Sun] [M/H] Model atmosphere metallicity ([M/H]model)
44- 48 F5.2 [Sun] [Fe/H] Derived stellar metallicity ([Fe/H]derived)
50 I1 --- C-rich [0-2]?=- Carbon-rich source code (C-rich) (2)
52 I1 --- CH [0-1]?=- Strong CH line source code (CH) (3)
54- 66 A13 --- Class Classification (Class) (4)
--------------------------------------------------------------------------------
Note (1): When SNR < 10, we report Teff, logg, and [Fe/H], but no chemical
abundance ratios.
Note (2): The source code is made as follows:
0 = C-normal
1 = CEMP object adopting the Aoki et al. (2007ApJ...655..492A 2007ApJ...655..492A,
Cat. J/ApJ/655/492) definition
2 = C-rich when including the Placco et al. (2014ApJ...797...21P 2014ApJ...797...21P,
Cat. J/ApJ/797/21) corrections for the effect of evolutionary
status on carbon abundances
Note (3): The source code is made as follows:
0 = G-band maximum depth is => 0.75 relative to the continuum
1 = G-band maximum depth in the best-fitting synthesis near
4323 Å is < 0.75 relative to the continuum
Note (4): The classification is as follows:
CEMP = carbon-enhanced metal-poor stars based on the carbon
abundance ratio ([C/Fe])
CEMP-no = not CEMP
NEMP = nitrogen-enhanced metal-poor stars based on the
nitrogen abundance ratio ([N/Fe])
Fe-rich = metal rich stars based on the iron abundance ratio
([Fe/H])
r-I = 'r-I' stars
r-II = 'r-II' srars
α-poor = α-poor stars based on the α abundance ratio
([α/Fe])
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- SMSS Star's name identifier (ID) (G1)
21 A1 --- Telescope [K/M] Telescope chosen for the obsvervations
(Telescope) (G2)
23 A1 --- l_A(C) Upper limit flag on A(C) abundance (l_AC)
25- 28 F4.2 [Sun] A(C) ?=- Carbon abundance relative to the sun
(AC) (1)
30- 33 F4.2 [Sun] Ccorr ?=- Carbon abundance correction for
evolutionary status (Ccorr) (2)
35 A1 --- l_[C/Fe]c Upper limit flag on [C/Fe]c (l_[C/Fe]c)
37- 41 F5.2 [Sun] [C/Fe]c ?=- Carbon to iron abundance ratio corrected
for evolutionary status ([C/Fe]corr) (2)
--------------------------------------------------------------------------------
Note (1): A(C) = 12 + log(NC/NH), A(H) = 12, abundance formula relative to
solar abundances adopted from Asplund at al. (2009ARA&A..47..481A 2009ARA&A..47..481A).
Note (2): Evolutionary corrections from Placco et al. (2014ApJ...797...21P 2014ApJ...797...21P,
Cat. J/ApJ/797/21).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- Species Species name identifier (Species) (1)
6- 24 A19 --- SMSS Star's name identifier (ID) (G1)
26 A1 --- Tel [K/M] Telescope chosen for the obsvervations
(Telescope) (G2)
28 A1 --- l_A(X) Upper limit flag on A(X) (l_AX)
30- 34 F5.2 [Sun] A(X) ?=- Element abundance relative to the sun
(AX) (2)
36- 38 I3 --- Nlines ?=- Number of lines measured (Nlines)
40- 43 F4.2 [Sun] e_A(X) ?=- Standard error of the mean A(X)
45 A1 --- l_[X/Fe] Upper limit flag on [X/Fe] (l_[X/Fe])
47- 51 F5.2 [Sun] [X/Fe] ?=- X element to iron abundance ratio
([X/Fe]) (3)
53- 56 F4.2 [Sun] eTot ?=- Total error updated with
max(e_A(X),0.20/sqrt(Nlines)) (Totalerror) (3)
--------------------------------------------------------------------------------
Note (1): The ionized species are : NaI, MgI, AlI, SiI, CaI, ScII, TiI, TiII,
CrI, MnI, FeI, FeII, CoI, NiI, SrII, BaII.
Note (2): A(X) = 12 + log(NX/NH), A(H) = 12, abundance formula relative to
solar abundances adopted from Asplund at al. (2009ARA&A..47..481A 2009ARA&A..47..481A).
Note (3): More details on abundance computations in the section 3 Analysis.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- Species Species name identifier (Species) (1)
6- 24 A19 --- SMSS Star's name identifier (ID) (G1)
26- 30 F5.2 [Sun] A(X) Element abundance relative to the sun (AX) (2)
32 I1 --- Nlines Number of lines measured (Nlines)
34- 37 F4.2 [Sun] e_A(X) ?=- Standard error of the mean A(X)
39- 43 F5.2 [Sun] [X/Fe] X element to iron abundance ratio ([X/Fe]) (3)
45- 48 F4.2 [Sun] eTot Total error updated with
max(e_A(X),0.20/sqrt(Nlines)) (Totalerror) (3)
--------------------------------------------------------------------------------
Note (1): The ionized species are : ZnI, YII, ZrII, EuII
Note (2): A(X) = 12 + log(NX/NH), A(H) = 12, abundance formula relative to
solar abundances adopted from Asplund at al. (2009ARA&A..47..481A 2009ARA&A..47..481A).
Note (3): More details on abundance computations in the section 3 Analysis.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table9.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- SMSS Star's name identifier (ID) (G1)
21 A1 --- Tel [K/M] Telescope chosen for the
obsvervations (Telescope) (G2)
23- 36 A14 --- Species Abundance ratio names (Species) (1)
38- 42 F5.2 100K DeltaTeff ?=- Effective temperature
uncertainty (DeltaTeff)
44- 48 F5.2 [cm/s2] Deltalogg ?=- Logaritm of the surface gravity
uncertainty by unit of 0.3dex (Deltalogg)
50- 54 F5.2 0.3km/s Deltavt ?=- Microturbulence velocity
uncertainty (Deltavt)
56- 60 F5.2 [Sun] Delta[M/H] ?=- Metallicity uncertainty by unit
of 0.3dex (Delta[M/H])
62- 68 F7.2 [Sun] Delta[X/Fe] ?=- X to iron abundance ratio
uncertainty (Delta[X/Fe])
--------------------------------------------------------------------------------
Note (1): The ionized species are : [FeI/H], [FeII/H], [Fe/H], [NaI/Fe],
[MgI/Fe], [AlI/Fe], [SiI/Fe], [CaI/Fe], [ScII/Fe], [TiI/Fe],
[TiII/Fe], [CrI/Fe], [MnI/Fe], [CoI/Fe], [NiI/Fe], [SrII/Fe],
[BaII/Fe].
--------------------------------------------------------------------------------
Byte-by-byte Description of file: sup.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- SMSS Star's name identifier (ID) (G1)
21- 24 I4 K Teff Effective temperature (Teff)
26- 29 F4.2 [cm/s2] logg Surface gravity (logg)
31- 35 F5.2 [Sun] [Fe/H] Iron abundance relative to the sun ([Fe/H])
37 I1 --- C-rich [0-2] Carbon-rich source code (C-rich) (1)
39- 42 F4.2 [Sun] Li ?=- Lithium abundance relative to the sun (Li)
44 A1 --- l_C Upper limit flag on C abundance (l_C)
46- 50 F5.2 [Sun] C ?=- Carbon abundance relative to the sun (C)
52- 56 F5.2 [Sun] N ?=- Nitrogen abundance relative to the sun (N)
58- 62 F5.2 [Sun] Na ?=- Sodium abundance relative to the sun (Na)
64- 68 F5.2 [Sun] Mg ?=- Magnesium abundance relative to the sun (Mg)
70- 74 F5.2 [Sun] Al ?=- Aluminium abundance relative to the sun (Al)
76- 79 F4.2 [Sun] Si ?=- Silicium abundance relative to the sun (Si)
81- 85 F5.2 [Sun] Ca ?=- Calcium abundance relative to the sun (Ca)
87- 91 F5.2 [Sun] Sc ?=- Scandium abundance relative to the sun (Sc)
93- 97 F5.2 [Sun] TiI ?=- Titanium abundance relative to the sun (TiI)
99-103 F5.2 [Sun] TiII ?=- Ionized Titanium abundance relative to
the sun (TiII)
105-109 F5.2 [Sun] Cr ?=- Chromium abundance relative to the sun (Cr)
111-115 F5.2 [Sun] Mn ?=- Manganese abundance relative to the sun (Mn)
117-121 F5.2 [Sun] FeI ?=- Iron abundance relative to the sun (FeI)
123-129 F7.2 [Sun] FeII ?=- Ionized Iron abundance relative to the
sun (FeII)
131-135 F5.2 [Sun] Co ?=- Cobalt abundance relative to the sun (Co)
137-141 F5.2 [Sun] Ni ?=- Nickel abundance relative to the sun (Ni)
143-147 F5.2 [Sun] Zn ?=- Zinc abundance relative to the sun (Zn)
149-153 F5.2 [Sun] Sr ?=- Strontium abundance relative to the sun (Sr)
155-159 F5.2 [Sun] Y ?=- Yttrium abundance relative to the sun (Y)
161-165 F5.2 [Sun] Zr ?=- Zirconium abundance relative to the sun (Zr)
167-171 F5.2 [Sun] Ba ?=- Barium abundance relative to the sun (Ba)
173-177 F5.2 [Sun] Eu ?=- Europium abundance relative to the sun (Eu)
--------------------------------------------------------------------------------
Note (1): The source code is made as follows:
0 = C-normal
1 = CEMP object adopting the Aoki et al. (2007ApJ...655..492A 2007ApJ...655..492A,
Cat. J/ApJ/655/492) definition
2 = C-rich when including the Placco et al. (2014ApJ...797...21P 2014ApJ...797...21P,
Cat. J/ApJ/797/21) corrections for the effect of evolutionary
status on carbon abundances
--------------------------------------------------------------------------------
Global notes:
Note (G1): SkyMapper DR1.1 (Wolf et al. 2018PASA...35...10W 2018PASA...35...10W, Cat. II/358)
Southern Survey designation of the form SMSS Jhhmmss.ss±ddmmss.s,
derived from mean ICRS coordinates (HHMMSS.s+DDMMSS.s).
Note (G2): Telescope name as follows:
F = ESO 2.2m telescope and FEROS spectrograph (Kaufer et al.
1999Msngr..95....8K 1999Msngr..95....8K)
K = Keck telescope and HIRES spectrograph (Vogt et al.
1994SPIE.2198..362V 1994SPIE.2198..362V)
M = Magellan Telescope and Magellan Inamori Kyocera Echelle (MIKE)
spectrograph (Bernstein et al. 2003SPIE.4841.1694B 2003SPIE.4841.1694B)
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 18-Jul-2024