Peak Frequency of the Synchrotron Emission and Classificatory Criteria of BL Lacertae Objects

Details Peak Frequency of the Synchrotron Emission and Classificatory Criteria of BL Lacertae Objects Peak Frequency of the Synchrotron Emission and Classificatory Criteria of BL Lacertae Objects

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002pasj...54..171d&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.54, No.2, pp.171-174

Astronomy and Astrophysics

Astronomy

3

Galaxies: Bl Lacertae Objects: General, Radiation Mechanism: Non-Thermal

Scientific paper

In this short paper, we quantitatively consider how the peak frequency of the synchrotron emission can be used to distinguish RBLs and XBLs. A sample of RBLs and XBLs presented by Sambruna etal. (1996, AAA065.159.120) was employed and the peak frequency, νp, of the synchrotron emission of each source was calculated by considering the proper physical origin of the X-ray emission for different classes of BLLac objects. A plot of αrx - log νp can be divided into four different regions by lines of αrx = 0.75 and log νp = 14.7 +/- 0.4. All RBL-like objects, defined by αrx > 0.75, are located in the upper-left region, while all XBL-like objects, defined by αrx <= 0.75, are inside the lower-right region. No sources are in the lower-left and upper-right regions, suggesting that the classificatory criteria in terms of the peak frequency should be l og νp = 14.7 +/- 0.4. This provides evidence supporting what Giommi etal. (1995, AAA063.158.163) proposed: RBL-like and XBL-like objects can be distinguished by the difference in the peak frequency of the synchrotron emission. The sometime confusing and observationally dependent RBL-XBL terminology should be replaced by the more physical LBL-HBL one.

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