Low-mass X-ray binary populations in galaxy outskirts: Globular clusters and supernova kicks

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Table 1

Galaxy sample.

Galaxy	D	Scale	r _e	b/a	PA	L _K	M_⋆/L_K	M _⋆	S _N	Age	Exp	/
	(Mpc)	(pc/arcsec)	(arcsec)		(degree)	(10¹⁰ L_K, ⊙)	(M_⊙/L_K, ⊙)	(10¹⁰ M_⊙)		(Gyr)	(ks)	(10³⁷ erg/s)
	(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)

N720	27.7	134	25.2	0.55	–40.0	21.50	0.86	18.49	1.01^a	3.4^aa	138.8	5.6/4.1
N821	24.1	117	19.6	0.62	30.0	9.12	0.82	7.48	1.14^b	5.2^bb	212.9	2.0/2.0
N1052	19.4	94	18.6	0.70	–60.0	8.94	0.80	7.15	1.59^c	14.5^cc	59.2	3.9/2.5
N1380	17.6	85	31.8	0.44	7.0	12.57	0.81	10.18	1.81^d	4.4^cc	41.6	3.5/2.9
N1404	21.0	102	18.6	0.90	–17.0	18.73	0.85	15.92	1.69^e	5.9^aa	114.5	5.7/2.9
N3115	9.7	47	33.6	0.39	45.0	9.43	0.83	7.83	2.22^f	8.4^bb	153.2	0.45/0.42
N3379	10.6	51	28.5	0.85	67.0	7.92	0.83	6.57	1.20^g	8.2^bb	337.0	0.33/0.33
N3585	20.0	97	29.9	0.63	–75.0	18.92	0.77	14.57	0.50^h	3.1^aa	94.7	2.6/2.7
N3923	22.9	111	40.5	0.64	47.0	29.90	0.82	24.52	3.57ⁱ	3.3^dd	102.1	3.6/3.4
N4125	23.9	116	31.4	0.63	82.0	23.49	0.80	18.79	1.30^h	5.0^ee	64.2	4.4/4.1
N4278	16.1	78	18.3	0.90	35.0	7.87	0.78	6.14	5.35^f	12.5^bb	470.8	0.62/0.60
N4365	20.4	99	38.1	0.74	45.0	20.86	0.85	17.73	3.95^j	7.9^bb	195.8	1.5/1.5
N4374	18.4	89	33.5	0.92	–57.0	24.94	0.83	20.70	5.39^k	9.8^cc	115.5	1.7/2.2
N4382	18.5	90	54.9	0.67	12.0	27.06	0.76	20.57	1.43^k	1.6^aa	39.7	2.9/4.1
N4472	16.3	79	56.1	0.81	–17.0	41.88	0.85	35.60	6.61^k	9.6^bb	89.6	3.2/3.7
N4552	15.3	74	22.8	0.94	–30.0	10.82	0.83	8.98	2.99^k	6.0^cc	54.4	1.8/1.8
N4636	14.7	71	56.2	0.84	–37.0	13.24	0.81	10.72	12.38^l	13.5^cc	209.8	1.4/1.4
N4649	16.8	81	42.1	0.81	–72.0	32.44	0.85	27.57	5.32^k	16.9^bb	108.0	2.3/2.3
N4697	11.7	57	39.5	0.63	67.0	8.82	0.77	6.79	3.78^m	10.0^cc	193.0	0.59/0.59
N5866	15.3	74	28.5	0.42	–57.0	9.47	0.72	6.82	1.69ⁿ	1.8^aa	33.7	2.1/1.9

Notes.(1) – Galaxy distance derived by Tonry et al. (2001). (2) – Scale conversion. (3), (4), and (5) – K_S-band half-light radius, axis-ratio, and position angle from the 2MASS Large Galaxy Atlas (Jarrett et al. 2003). (6) – Total K_S-band luminosity calculated from the total apparent K_S-band magnitude. (7) – K_S-band mass-to-light ratios derived from Bell & de Jong (2001), with B − V colors from RC3 catalog (de Vaucouleurs et al. 1991). (8) – Total stellar mass calculated from K_S-band total luminosity and the K_S-band mass-to-light ratio. (9) – Globular cluster specific frequencies derived following Zhang et al. (2012). References for the number of observed globular clusters in each galaxy are – (10) – Stellar age of the galaxy. References – (11) – Total exposure time of the combined Chandra observations. (12) – Limiting source detection sensitivity in the 0.5−8 keV band in the (0.2–3)r_e () and outer (4–10)r_e () regions.

^(a)

Kissler-Patig et al. (1996);

^(b)

Spitler et al. (2008);

^(c)

Forbes et al. (2001);

^(d)

Kissler-Patig et al. (1997);

^(e)

Forbes et al. (1998);

^(f)

Harris (1991);

^(g)

Rhode & Zepf (2004);

^(h)

Humphrey (2009);

⁽ⁱ⁾

Sikkema et al. (2006);

^(j)

Forbes (1996);

^(k)

Peng et al. (2008);

^(l)

Dirsch et al. (2005);

^(m)

Dirsch (1996);

⁽ⁿ⁾

Cantiello et al. (2007).

^(aa)

Terlevich & Forbes (2002);

^(bb)

Sánchez-Blázquez et al. (2006);

^(cc)

Annibali et al. (2007);

^(dd)

Thomas et al. (2005);

^(ee)

Schweizer & Seitzer (1992).

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