Highly variable AGN from the XMM-Newton slew survey

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Table B.3

Allowed column densities of ionised gas.

XMMSL1 name	Obs. date	C _red	Spectral	Ionisation^a	N_H,max ^b	Implied^c	Observed^d	Can it explain
			index		(10²⁰ cm^-2)	flux change	flux change	variability?

J005953.1+314934	2011-08-28	1.07	1.7^e	low	5.1	1.2	1.9	no
J020303.1-074154	2010-03-01	0.74	1.7^e	high	69	3.3	5.8	no
J024916.6-041244	2007-06-27	1.03	1.7^e	high^f	150	110	17	yes
J044347.0+285822	2010-07-27	1.05	1.7^e	low	210	260	7.3	yes
J045740.0-503053	2010-10-03	0.99	1.7^e	medium	72	2.5	17	no
J064541.1-590851	2010-12-26	0.77	2.0	high	190	1.6	1.4	yes
J082753.7+521800	2010-03-11	1.13	2.3	high	650	3.2	2.7	yes
J090421.2+170927	2010-06-12	0.83	1.7^e	high	1400	7.3	3.6	yes
J093922.5+370945	2011-03-28	1.20	3.2	low	9.9	2.2	3.4	no
J100534.8+392856	2011-01-01	1.22	1.7^e	high	180	1.5	1.7	maybe
J104745.6-375932	2010-04-11	0.88	2.2	high	700	1.7	1.6	yes
J112841.5+575017	2011-03-01	0.74	1.7^e	high	7.0	3.1	–	Swift point brightest
J121335.0+325609	2006-06^g	0.99	1.5	low	7.9	1.3	4.9	no
J162553.4+562735	2010-07-10	0.89	2.2	low	13	1.9	3.2	no
J173739.3-595625	2008-11-02	0.91	2.0	high	140	1.4	2.0	no
J183521.4+611942	2011-02-01	1.51	1.7^e	high	610	1.6	5.4	no

Notes.

^(a)

Ionisation level which yields largest flux change: low (log(ξ) = −1); medium (log(ξ) = 0.5); high (log(ξ) = 2).

^(b)

Maximum ionised hydrogen column allowed by power law fit to the Swift spectrum (90% confidence).

^(c)

Fractional change in observed 0.2–2 keV flux due to this N_H column.

^(d)

Change in 0.2–2 keV flux actually observed between the highest flux measurement and the Swift observation.

^(e)

Power law slope fixed at 1.7 during fit.

^(f)

A medium ionisation level yields even stronger absorption, however the fit is worse.

^(g)

Merged spectra taken between 2006-06-02 and 2006-06-12.

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