Table 1: Basic properties of Seyfert-type warm absorbers observed with XMM-Newton and Chandra: object name, morphological type, redshift, log $L_{\rm bol}$ (erg s $^{\rm -1}$ ; with reference if different to that given in the last column), whether the X-ray spectrum is dominated by emission lines (EM), whether the source has a warm absorber (WA), whether a detailed spectral model has been published (Mod), whether the warm absorber is outflowing (Outflow), and reference for the warm absorber model.
Object Type z log $L_{\rm bol}$ EM WA Mod Outflow Reference

MR2251-178 Sy1 RQQ 0.06398 45.7^a $\bullet$ $\bullet$ $\bullet$ Kaspi et al. (2003)

PG0844+349 Sy1 RQQ 0.064 45.5 $\bullet$ $\bullet$ $\bullet$ Pounds et al. (2003a)

PG1211+143 NLSy1 RQQ^p 0.0809 45.6 $\bullet$ $\bullet$ $\bullet$ Pounds et al. (2003b)

PKS 0558-504 NLSy1 RLQ 0.137 $\sim$ 46 O'Brien et al. (2001b)

IRAS 13349+2438 NLSy1 RQQ 0.10764 46.4^b $\bullet$ $\bullet$ $\bullet$ Sako et al. (2001)

ESO 141-G55 Sy1 0.036 $\sim$ 45 Gondoin et al. (2003)

NGC 4593 Sy1 0.0084 43.5^c $\bullet$ $\bullet$ $\bullet$ Steenbrugge et al. (2003a)

NGC 3783 Sy1 0.00973 44.7^d $\bullet$ $\bullet$ $\bullet$ Netzer et al. (2003)

Markarian 509 Sy1.2 0.0344 $\geq$ 45.5^e $\bullet$ $\bullet$ $\bullet$ Yaqoob et al. (2003)

NGC 7469 Sy1.2 0.0164 44.4^f $\bullet$ $\bullet$ $\bullet$ Blustin et al. (2003)

Markarian 279 Sy1.5 0.0305 $\sim$ 45^g Scott et al. (2004)

NGC 3516 Sy1.5 0.009 $\sim$ 44 $\bullet$ $\bullet$ $\bullet$ Netzer et al. (2002)

NGC 5548 Sy1.5 0.01676 44.7^h $\bullet$ $\bullet$ $\bullet$ Steenbrugge et al. (2003b)

NGC 4151 Sy1.5 0.00332 $\sim$ 44ⁱ $\bullet$ Schurch et al. (2004)

NGC 5506 Sy1.9 0.00618 $\sim$ 44 $\bullet$ Bianchi et al. (2003)

NGC 4258 Sy1.9 LINER 0.00149 $\sim$ 42^j $\bullet$ $\bullet$ Young & Wilson (2004)

Markarian 478 NLSy1 0.079^k 45.2^k Marshall et al. (2003)

Ton S180 NLSy1 0.06198 $\sim$ 46^l $\bullet$ Rózanska et al. (2004)

MCG -6-30-15 NLSy1 0.00775 $\sim$ 44^m $\bullet$ $\bullet$ $\bullet$ Sako et al. (2003)

Markarian 766 NLSy1 0.012929 $\sim$ 44ⁿ $\bullet$ $\bullet$ Mason et al. (2003)

NGC 4051 NLSy1 0.00234 43.4 $\bullet$ $\bullet$ $\bullet$ Ogle et al. (2004)

Markarian 359 NLSy1 0.0174 $\sim$ 44 $\bullet$ ? O'Brien et al. (2001a)

Ark 564 NLSy1 0.02468 44.4^o $\bullet$ $\bullet$ $\bullet$ Matsumoto et al. (2004)

^a Monier et al. (2001); ^b Beichman et al. (1986); ^c Santos-Lleo et al. (1995); ^d Markowitz et al. (2003); ^e Kriss et al. (2000); ^f Petrucci et al. (2004); ^g Bachev & Strigachev (2003); ^h Pounds et al. (2003c); ⁱ Swain et al. (2003); ^j Yuan et al. (2002); ^k Gondhalekar et al. (1994); ^l Turner et al. (2002); ^m Reynolds (2000); ⁿ Pounds et al. (2003d); ^o Romano et al. (2002); ^p Kaspi et al. (2000b).

**Table 1:** Basic properties of Seyfert-type warm absorbers observed with XMM-Newton and Chandra: object name, morphological type, redshift, log $L_{\rm bol}$ (erg s $^{\rm -1}$ ; with reference if different to that given in the last column), whether the X-ray spectrum is dominated by emission lines (EM), whether the source has a warm absorber (WA), whether a detailed spectral model has been published (Mod), whether the warm absorber is outflowing (Outflow), and reference for the warm absorber model.
Object	Type	z	log $L_{\rm bol}$	EM	WA	Mod	Outflow	Reference
MR2251-178	Sy1 RQQ	0.06398	45.7^a		$\bullet$	$\bullet$	$\bullet$	Kaspi et al. (2003)
PG0844+349	Sy1 RQQ	0.064	45.5		$\bullet$	$\bullet$	$\bullet$	Pounds et al. (2003a)
PG1211+143	NLSy1 RQQ^p	0.0809	45.6		$\bullet$	$\bullet$	$\bullet$	Pounds et al. (2003b)
PKS 0558-504	NLSy1 RLQ	0.137	$\sim$ 46					O'Brien et al. (2001b)
IRAS 13349+2438	NLSy1 RQQ	0.10764	46.4^b		$\bullet$	$\bullet$	$\bullet$	Sako et al. (2001)
ESO 141-G55	Sy1	0.036	$\sim$ 45					Gondoin et al. (2003)
NGC 4593	Sy1	0.0084	43.5^c		$\bullet$	$\bullet$	$\bullet$	Steenbrugge et al. (2003a)
NGC 3783	Sy1	0.00973	44.7^d		$\bullet$	$\bullet$	$\bullet$	Netzer et al. (2003)
Markarian 509	Sy1.2	0.0344	$\geq$ 45.5^e		$\bullet$	$\bullet$	$\bullet$	Yaqoob et al. (2003)
NGC 7469	Sy1.2	0.0164	44.4^f		$\bullet$	$\bullet$	$\bullet$	Blustin et al. (2003)
Markarian 279	Sy1.5	0.0305	$\sim$ 45^g					Scott et al. (2004)
NGC 3516	Sy1.5	0.009	$\sim$ 44		$\bullet$	$\bullet$	$\bullet$	Netzer et al. (2002)
NGC 5548	Sy1.5	0.01676	44.7^h		$\bullet$	$\bullet$	$\bullet$	Steenbrugge et al. (2003b)
NGC 4151	Sy1.5	0.00332	$\sim$ 44ⁱ	$\bullet$				Schurch et al. (2004)
NGC 5506	Sy1.9	0.00618	$\sim$ 44	$\bullet$				Bianchi et al. (2003)
NGC 4258	Sy1.9 LINER	0.00149	$\sim$ 42^j	$\bullet$	$\bullet$			Young & Wilson (2004)
Markarian 478	NLSy1	0.079^k	45.2^k					Marshall et al. (2003)
Ton S180	NLSy1	0.06198	$\sim$ 46^l		$\bullet$			Rózanska et al. (2004)
MCG -6-30-15	NLSy1	0.00775	$\sim$ 44^m		$\bullet$	$\bullet$	$\bullet$	Sako et al. (2003)
Markarian 766	NLSy1	0.012929	$\sim$ 44ⁿ		$\bullet$	$\bullet$		Mason et al. (2003)
NGC 4051	NLSy1	0.00234	43.4		$\bullet$	$\bullet$	$\bullet$	Ogle et al. (2004)
Markarian 359	NLSy1	0.0174	$\sim$ 44		$\bullet$		?	O'Brien et al. (2001a)
Ark 564	NLSy1	0.02468	44.4^o		$\bullet$	$\bullet$	$\bullet$	Matsumoto et al. (2004)

Source LaTeX | All tables | In the text

	1 Introduction
	2 Data and analysis
	3 Results and discussion
	4 Conclusions
	References