Dust grain growth in the interstellar medium of 5 < z < 6.5 quasars

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Table 1

Dust, gas and dynamical masses of z > 5 QSOs.

			M_dust	M_gas	M_dynsin²i		T_dust
No.	QSO	z	(10⁸M_⊙)	(10¹⁰M_⊙)	(10¹⁰M_⊙)		(K)

1	J0338+0021	5.03	7.1 ± 0.6	2.2^a	3.0^a	31	45.6^d>
2	J0840+5624	5.85	4.7 ± 0.9	2.5^b	24.2^b	53	...
3	J0927+2001	5.77	7.2 ± 1.1	1.8^b	11.8^b	25	51.1^d
4	J1044 − 0125	5.74	2.7 ± 0.6	0.7^b	0.8^b	26	...
5	J1048+4637	6.23	4.3 ± 0.6	1.0^b	4.5^b	23	<40^e
6	J1148+5251	6.42	5.9 ± 0.7	1.6^c	4.5^c	27	55.0^f
7	J1335+3533	5.93	3.4 ± 0.7	1.8^b	3.1^b	53	...
8	J1425+3254	5.85	3.3 ± 0.7	2.0^b	15.6^b	60	...
9	J2054 − 0005	6.06	3.4 ± 0.8	1.2^b	4.2^b	35	...

Notes. The sample includes QSOs detected in their dust continuum and CO line emission (Carilli et al. 2000, 2001, 2007; Bertoldi et al. 2003a,b; Petric et al. 2003; Priddey et al. 2003, 2008; Walter et al. 2003, 2004; Robson et al. 2004; Beelen et al. 2006; Maiolino et al. 2007; Riechers et al. 2007; Wang et al. 2007, 2008a,b, 2010; Wu et al. 2009). We calculated dust masses from the detection of 1200μm emission using Eq. (5) of Michałowski et al. (2009) assuming β = 1.3. The errors reflect the statistical uncertainties only. For three QSOs we assumed observationally inferred dust temperatures (the last column). For the rest we adopted the average of these estimates T_dust = 50 K.

^(a)

Maiolino et al. (2007).

^(b)

Wang et al. (2010).

^(c)

Walter et al. (2004).

^(d)

Wang et al. (2008b).

^(e)

Robson et al. (2004).

^(f)

Beelen et al. (2006).

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