|[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|
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
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).
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