Table 1:

Physical properties observed in X-ray-emitting HH jets.

object		cnts					D	LM/HM	Reference
	[ks]		[1029 erg s-1]	[106 K]	[arcsec]	[AU]	[pc]
HH 2	21.4	11	5.2	1	2	56 000c	480	LM	Pravdo et al. (2001)
HH 154	97	63	3	4	5	70-140	140	LM	Favata et al. (2006)d
HH 80/81	37.3	46/63	450/430	1.5	-	515 000	1700	HM	Pravdo et al. (2004)
HH 168	78	-	30	6.5	-	-	730	HM	Pravdo et al. (2009)
HH 210	838	31	10	0.8	-	37 000c	450	HM	Grosso et al. (2006)
HH 540	795.8	200	0.4	6.6	-	<90	450	LM	Kastner et al. (2005)a
HH 216	78	8	10	-	4	-	2000	-	Linsky et al. (2007)
DG Tau	90	18; 9b	0.12	3.4	5	30	140	LM	Güdel et al. (2008)
Z CMa	39.6	20	>2.6	2.3	-	>2000	1050	HM	Stelzer et al. (2009)
TKH 8	89.2	28	20	35.4	-	450-900	450	LM	Tsujimoto et al. (2004)e

Notes.  is the exposure time of the observations (or the total exposure time adding together several observations, as in the case of DG Tau); cnts are the collected photons; is the X-ray luminosity roughly in the [0.3-10] keV band; is the best fit temperature; is the linear size of the X-ray source; is the distance of the X-ray source from the central protostar; D is the distance of the HH object; LM/HM indicates the low-mass or high-mass young stellar object from which the jet originates.
^(a) Improved estimates of and from Joel Kastner and Ettore Flaccomio, private communication.
^(b) The first value is associated with the South-Western jet and the second with the North-Eastern jet in DG Tau.
^(c) Values derived from SIMBAD.
^(d) See also Bally et al. (2003).
^(e) See also Tsuboi et al. (2001).