The present-day cosmic phosphorus abundance | Astronomy & Astrophysics (A&A)

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Table B.1

Properties of the sample stars and non-LTE phosphorus abundances.

#	Object	Sp. Type	Instrument	Teff K	log g (cgs)	ξ	u sin i	ζ	Ref.	d^a pc	logP/H+12

						km s^-1
late O-type stars:
	HD 34078	O9.5 V	FOCES/UVES	33200±300	4.06±0.05	8±2	9±2	23±3	1	380 $_{- 5}^{+ 5}$ $^{+5}_{-5}$	5.40±0.03 (3)
	HD 36512	O9.7 V	FOCES/UVES	32900±600	4.20±0.05	7±2	8±4	26±4	1	408 $_{- 27}^{+ 23}$ $^{+23}_{-27}$	5.35±0.05 (3)
	HD 46202	O9.2 V	FEROS/UVES	33900±500	4.16±0.05	6±2	11±1	33±4	1	1442 $_{- 180}^{+ 685}$ $^{+685}_{-180}$	5.30±0.03 (3)
	HD 54879	O9.7 V	FEROS	32200±700	4.06±0.05	4±2	0±1	0±1	1	1198 $_{- 41}^{+ 45}$ $^{+45}_{-41}$	5.27 (1)
	HD 57682	O9.2 IV	UVES	33500±800	3.93±0.05	4±2	10±1	33±4	1	1106 $_{- 82}^{+ 111}$ $^{+111}_{-82}$	5.30±0.07 (3)
	HD 206183	O9.5 V	FOCES	33100±300	4.06±0.05	4±2	4±2	21±4	1	903 $_{- 15}^{+ 14}$ $^{+14}_{-15}$	5.18 (1)
	HD 207538	O9.7 IV	ESPaDOnS	31400±500	3.93±0.05	8±2	32±3	42±3	1	834 $_{- 10}^{+ 11}$ $^{+11}_{-10}$	5.36 (1)
	HD 214680	O9 V	FOCES	34550±300	4.04±0.05	5±2	14±1	32±2	1	454 $_{- 32}^{+ 25}$ $^{+25}_{-32}$	5.25 (1)
	BD -13 4930	O9.5 V	ESPaDOnS	32900±300	4.14±0.05	6±2	8±2	23±4	1	1579 $_{- 46}^{+ 45}$ $^{+45}_{-46}$	5.41 (1)
early B-type stars:
	HD 886	B2 IV	FOCES	22000±400	3.95±0.05	2±1	9±2	8±2	2	146 $_{- 8}^{+ 10}$ $^{+10}_{-8}$	5.25±0.02 (3)
	HD 3360	B2 IV	FIES	20750±200	3.80±0.05	2±1	20±2	12±5	2	150 $_{- 8}^{+ 7}$ $^{+7}_{-8}$	5.42±0.07 (3)
	HD 16582	B2 IV	CAFE	21250±400	3.80±0.05	2±1	15±2	10±5	2	194 $_{- 9}^{+ 10}$ $^{+10}_{-9}$	5.45±0.10 (2)
	HD 34816	B0.5 IV	FEROS	30000±300	4.15±0.08	4±1	25±2	32±7	2^b	298 $_{- 14}^{+ 19}$ $^{+19}_{-14}$	5.67±0.05 (3)
	HD 35039	B2 V	FIES	19600±200	3.56±0.07	4±1	12±1	7±1	3	350 $_{- 16}^{+ 22}$ $^{+22}_{-16}$	5.31±0.06 (5)
	HD 35299	B1.5 V	FOCES	23500±300	4.20±0.05	0±1	8±1	...	2	356 $_{- 11}^{+ 12}$ $^{+12}_{-11}$	5.18±0.06 (3)
	HD 35708	B2.5 IV	FOCES	20700±200	4.15±0.07	2±1	25±2	17±5	2	185 $_{- 4}^{+ 5}$ $^{+5}_{-4}$	5.46±0.01 (3)
	HD 35912	B2 V	FIES	19800±400	4.20±0.10	0±1	8±4	18±5	3^b	365 $_{- 9}^{+ 10}$ $^{+10}_{-9}$	5.30±0.02 (2)
	HD 36285	B2 V	FIES	21700±300	4.25±0.08	0±1	11±1	8±1	3	351 $_{- 7}^{+ 7}$ $^{+7}_{-7}$	5.39±0.09 (3)
	HD 36591	B1 V	FEROS	27000±300	4.12±0.05	3±1	12±1	...	2	425 $_{- 31}^{+ 36}$ $^{+36}_{-31}$	5.25±0.03 (3)
	HD 36629	B2 V	FIES	20300±400	4.15±0.10	2±1	10±1	5±1	3	424 $_{- 6}^{+ 8}$ $^{+8}_{-6}$	5.30±0.03 (3)
	HD 36822	B0 III	FOCES/UVES	30000±300	4.05±0.10	8±1	28±2	18±5	2	374 $_{- 36}^{+ 45}$ $^{+45}_{-36}$	5.48±0.08 (3)
	HD 36959	B1 V	FIES	26100±200	4.25±0.07	0±1	12±1	5±1	3	358 $_{- 14}^{+ 15}$ $^{+15}_{-14}$	5.24±0.03 (2)
	HD 37042	B0.7 V	FIES	29300±300	4.30±0.09	2±1	30±2	10±3	3	413 $_{- 8}^{+ 11}$ $^{+11}_{-8}$	5.52 (1)
	HD 37744	B1.5 V	FIES	24600±300	4.20±0.05	0±1	37±1	3±2	3^b	389 $_{- 12}^{+ 10}$ $^{+10}_{-12}$	5.13±0.02 (2)
	HD 44743	B1 II/III	FEROS	24300±500	3.60±0.05	8±1	30±2	32±3	4^b	151 $_{- 5}^{+ 5}$ $^{+5}_{-5}$	5.12±0.04 (2)
	HD 63922	B0 III	FEROS	31200±300	3.95±0.05	8±1	29±4	37±8	2	297 $_{- 31}^{+ 52}$ $^{+52}_{-31}$	5.37 (1)
	HD 122980	B2 V	FEROS	20800±300	4.22±0.05	3±1	18±1	...	2	153 $_{- 5}^{+ 5}$ $^{+5}_{-5}$	5.21±0.03 (3)
	HD 149438	B0.2 V	FEROS/UVES	32000±300	4.30±0.05	5±1	4±1	4±1	2	145 $_{- 10}^{+ 12}$ $^{+12}_{-10}$	5.38±0.08 (4)
	HD 160762	B3 IV	FIES	17500±200	3.80±0.05	1±1	6±1	...	2	153 $_{- 4}^{+ 6}$ $^{+6}_{-4}$	5.40±0.13 (9)
	HD 205021	B1 IV	FOCES	27000±450	3.95±0.05	4±1	28±3	20±7	2	210 $_{- 12}^{+ 14}$ $^{+14}_{-12}$	5.41 (1)
	HD 209008	B3 III	FOCES	15800±200	3.75±0.05	4±1	15±3	10±3	2	459 $_{- 19}^{+ 22}$ $^{+22}_{-19}$	5.56±0.05 (4)
	HD 216916	B2 IV	FOCES	23000±200	3.95±0.05	0±1	12±1	...	2	441 $_{- 14}^{+ 18}$ $^{+18}_{-14}$	5.26 (1)
B-type supergiants:
	HD 14818	B2 Ia	FOCES	18600±300	2.45±0.07	14±2	48±6	40±5	6	2121 $_{- 107}^{+ 145}$ $^{+145}_{-107}$	5.16 (1)
	HD 34085	B8 Ia	FEROS	12000±200	1.75±0.10	7±1	36±5	22±5	5	265 $_{- 22}^{+ 26}$ $^{+26}_{-22}$	5.53±0.07 (6)
	HD 51309	B3 Ib	FEROS	15600±400	2.59±0.05	10±2	30±6	35±5	6	1108 $_{- 215}^{+ 407}$ $^{+407}_{-215}$	5.30±0.23 (4)
	HD 119646	B1.5 Ib	FEROS	19700±200	2.90±0.07	14±2	37±6	40±5	6	1721 $_{- 73}^{+ 84}$ $^{+84}_{-73}$	5.06 (1)
	HD 125288	B5 II	FEROS	13700±300	2.77±0.05	6±2	23±4	30±5	6	438 $_{- 30}^{+ 51}$ $^{+51}_{-30}$	5.63±0.04 (3)
	HD 159110	B2 II	FEROS	19500±300	3.42±0.05	3±2	17±4	15±5	6	1362 $_{- 71}^{+ 80}$ $^{+80}_{-71}$	5.27±0.02 (3)
	HD 164353	B5 Ib	FEROS	14700±300	2.57±0.05	8±2	20±4	32±5	6	797 $_{- 129}^{+ 196}$ $^{+196}_{-129}$	5.33±0.06 (3)
	HD 183143	B7 Ia	FOCES	12800±200	1.76±0.05	7±2	37±5	27±5	6	2168 $_{- 122}^{+ 119}$ $^{+119}_{-122}$	5.59±0.05 (2)
	HD 184943	B8 Iab	FOCES	11900±200	1.88±0.05	9±2	35±6	25±5	6	4090 $_{- 236}^{+ 236}$ $^{+236}_{-236}$	5.52 (1)
	HD 191243	B5 Ib	FOCES	14000±300	2.64±0.06	8±2	27±6	25±5	6	1205 $_{- 32}^{+ 32}$ $^{+32}_{-32}$	5.56±0.05 (4)

References. (1) Aschenbrenner et al. (2023); (2) Nieva & Przybilla (2012); (3) Nieva & Simón-Díaz (2011); (4) Fossati et al. (2015); (5) Przybilla et al. (2006); (6) Weßmayer et al. (2022).

Notes. The number in brackets at the end of each row gives the number of phosphorus lines analysed. ^(a) Gaia Collaboration (2016, 2021) photogeometric distances and associated 14th and 86th confidence percentiles (Bailer-Jones et al. 2021); for HD 36591, HD 36822 and HD 36959 inverse parallax distances based on Gaia Collaboration (2023) data; for HD 149438, HD 205021, HD 44743 and HD 34085 inverse parallax distances based on van Leeuwen (2007) data. ^(b) The atmospheric parameters of these stars were refined in this work. If available, the iron abundances to be used in Fig. 6 were adopted from the original references.

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