Pulsating hot O subdwarfs in ω Centauri: mapping a unique instability strip on the extreme horizontal branch

S. K. Randall; A. Calamida; G. Fontaine; M. Monelli; G. Bono; M. L. Alonso; V. Van Grootel; P. Brassard; P. Chayer; M. Catelan; S. Littlefair; V. S. Dhillon; T. R. Marsh

doi:10.1051/0004-6361/201528006

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Volume 589 (May 2016)

A&A, 589 (2016) A1

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Table 5

Atmospheric parameters inferred for our FORS2 spectroscopic sample of 47 EHB stars with clean or slightly polluted spectra.

	T_eff (K)	log g	log (He/H)	Ref.	B _ACS/WFI	R_ACS/V_WFI	Phot.	Det. (%)

177614	56 404 ± 722	6.184 ± 0.070	−1.476 ± 0.085	ACS	18.443 ± 0.011	18.699 ± 0.012	efosc4	0.46
281063	53 393 ± 1190	6.102 ± 0.092	−1.655 ± 0.134	ACS	18.506 ± 0.013	18.719 ± 0.013	ucam	0.31	V5
154681	51 990 ± 745	5.828 ± 0.073	−1.242 ± 0.051	WFI	18.205 ± 0.003	18.415 ± 0.003	efosc5	0.73	V4
172409^∗	50 862 ± 1127	5.643 ± 0.065	−2.390 ± 0.136	ACS	18.151 ± 0.015	18.456 ± 0.016	efosc9	1.08
260664^∗	49 858 ± 863	5.542 ± 0.054	−1.841 ± 0.073	ACS	18.438 ± 0.012	18.638 ± 0.011	ucam	0.36	V2
177238	49 277 ± 886	6.014 ± 0.069	−1.719 ± 0.100	ACS	18.300 ± 0.012	18.583 ± 0.016	efosc4	0.77	V3
5034421	48 500 ± 622	5.798 ± 0.046	−1.819 ± 0.060	ACS	18.299 ± 0.013	18.547 ± 0.012	ucam	0.25	V1
248955^∗	48 209 ± 1009	5.445 ± 0.083	−1.330 ± 0.082	ACS	18.014 ± 0.014	18.192 ± 0.013	ucam	0.38	SV
5128088^∗	47 748 ± 893	5.993 ± 0.093	−1.197 ± 0.077	WFI	18.816 ± 0.003	18.985 ± 0.003	ucam	0.53	135227^∗∗
5143191^∗	47 552 ± 984	5.475 ± 0.082	−1.388 ± 0.081	ACS	18.137 ± 0.021	18.339 ± 0.043	ucam	0.63
5067230^∗	45 351 ± 688	5.740 ± 0.107	−0.539 ± 0.074	ACS	18.692 ± 0.010	18.892 ± 0.011	ucam	1.29
165237	44 456 ± 377	6.178 ± 0.110	1.017 ± 0.158	ACS	18.335 ± 0.011	18.546 ± 0.011	no
5242616	43 601 ± 626	5.862 ± 0.076	−1.502 ± 0.074	WFI	18.427 ± 0.004	18.551 ± 0.005	no
5039935	39 815 ± 464	6.085 ± 0.107	0.556 ± 0.076	ACS	19.160 ± 0.023	19.314 ± 0.019	ucam	0.65
5138707	39 359 ± 381	6.110 ± 0.089	0.617 ± 0.059	ACS	19.094 ± 0.013	19.293 ± 0.014	no
5085696	38 757 ± 364	5.711 ± 0.084	−0.102 ± 0.053	WFI	18.747 ± 0.003	18.744 ± 0.004	no
5047695	38 724 ± 545	5.819 ± 0.119	−0.237 ± 0.077	ACS	18.968 ± 0.032	19.122 ± 0.026	ucam	0.37
5124244	38 248 ± 506	6.011 ± 0.094	−0.041 ± 0.056	WFI	18.892 ± 0.004	19.033 ± 0.004	ucam	0.43
5170422	38 183 ± 321	5.775 ± 0.061	−0.773 ± 0.044	WFI	18.352 ± 0.003	18.454 ± 0.004	ucam	0.31
177711	36 984 ± 422	5.783 ± 0.073	−0.530 ± 0.052	ACS	18.591 ± 0.014	18.796 ± 0.014	efosc4	0.48
264057	36 645 ± 392	5.833 ± 0.069	−0.885 ± 0.053	ACS	18.583 ± 0.016	18.777 ± 0.013	ucam	0.58
5059328^∗	36 506 ± 544	5.647 ± 0.099	−0.654 ± 0.072	ACS	18.874 ± 0.024	19.075 ± 0.019	ucam	1.3
5142638	36 481 ± 401	5.791 ± 0.067	−0.477 ± 0.047	WFI	18.811 ± 0.003	18.919 ± 0.003	efosc7	3.92
5220684	36 442 ± 332	5.932 ± 0.057	−0.909 ± 0.044	ACS	18.500 ± 0.014	18.727 ± 0.013	efosc4	0.69
5062474	36 438 ± 888	5.904 ± 0.139	−0.116 ± 0.085	ACS	18.919 ± 0.021	18.938 ± 0.040	ucam	1.2
5102280	36 395 ± 317	5.717 ± 0.056	−0.949 ± 0.043	WFI	18.357 ± 0.002	18.441 ± 0.003	no
165943	36 261 ± 344	5.847 ± 0.060	−0.745 ± 0.043	ACS	18.513 ± 0.015	18.764 ± 0.015	no
274052	36 191 ± 486	5.656 ± 0.083	−0.389 ± 0.058	ACS	18.720 ± 0.014	18.883 ± 0.013	ucam	0.36
5242504	36 072 ± 379	5.807 ± 0.066	−0.532 ± 0.048	WFI	18.657 ± 0.003	18.824 ± 0.004	no
5164025	36 036 ± 391	5.890 ± 0.070	−0.646 ± 0.050	WFI	18.878 ± 0.003	19.037 ± 0.004	ucam	0.36
5165122	35 876 ± 321	5.783 ± 0.056	−0.719 ± 0.041	WFI	18.601 ± 0.003	18.775 ± 0.003	ucam	0.32
5205350	35 837 ± 328	5.539 ± 0.056	−0.699 ± 0.043	WFI	18.462 ± 0.003	18.616 ± 0.003	no
5141232	35 804 ± 356	5.686 ± 0.065	−0.677 ± 0.046	WFI	18.578 ± 0.003	18.739 ± 0.003	ucam	0.35
75981	35 122 ± 288	5.789 ± 0.049	−1.107 ± 0.041	WFI	18.313 ± 0.003	18.513 ± 0.003	no		75981^∗∗
53945	34 860 ± 333	5.959 ± 0.056	−0.711 ± 0.040	WFI	18.724 ± 0.003	18.906 ± 0.003	efosc2	0.71	53945^∗∗
5119720	34 775 ± 394	5.836 ± 0.066	−0.861 ± 0.050	ACS	18.619 ± 0.013	18.778 ± 0.013	ucam	0.33
5222459	34 668 ± 290	5.793 ± 0.048	−0.722 ± 0.036	WFI	18.825 ± 0.003	18.952 ± 0.003	efosc2	0.81
5180753	34 140 ± 283	5.783 ± 0.049	−1.490 ± 0.051	ACS	18.400 ± 0.012	18.599 ± 0.016	efosc9	1.18
5142999	33 843 ± 380	5.641 ± 0.061	−1.155 ± 0.056	WFI	18.549 ± 0.003	18.735 ± 0.003	ucam	0.27	164808^∗∗
5243164	31 614 ± 245	5.408 ± 0.040	−2.656 ± 0.134	WFI	18.206 ± 0.003	18.359 ± 0.004	no		75993^∗∗
168035	31 458 ± 431	5.626 ± 0.070	−3.614 ± 0.557	ACS	17.929 ± 0.010	18.084 ± 0.011	no
5185548^∗	31 191 ± 338	5.546 ± 0.056	−4.365 ± 1.064	WFI	18.116 ± 0.002	18.251 ± 0.002	ucam	0.24
5262593	30 762 ± 255	5.497 ± 0.042	−3.393 ± 0.417	WFI	17.810 ± 0.002	17.938 ± 0.002	no
175411^∗	29 213 ± 293	5.454 ± 0.047	−3.176 ± 0.292	ACS	18.698 ± 0.016	18.713 ± 0.031	efosc9	1.62
204071	28 761 ± 657	5.570 ± 0.095	−3.074 ± 0.186	ACS	17.929 ± 0.021	18.100 ± 0.014	no
5139614	27 894 ± 379	5.521 ± 0.058	−3.758 ± 1.185	ACS	18.823 ± 0.012	18.934 ± 0.010	ucam	0.63
5238307	27 108 ± 261	5.512 ± 0.039	−2.287 ± 0.073	ACS	18.590 ± 0.013	18.673 ± 0.018	no

Notes. Also listed are the ACS/WFI B and R/V magnitudes. For the targets that overlap with our time-series photometry sample, the detection limit above which pulsations would have been detected is given. The rapid variables V1-V5 are indicated, as is the slow variable (SV).

^(∗)

Spectrum polluted by cooler star. The estimate of log g should be seen as a lower limit only.

^(∗∗)

ID from Moehler et al. (2011).

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