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IAUC 8068: 2003ag, 2003ah,, 2003ai; FLARING OBJECT IN Ori CLUSTER

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                                                  Circular No. 8068
Central Bureau for Astronomical Telegrams
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
URL http://cfa-www.harvard.edu/iau/cbat.html  ISSN 0081-0304
Phone 617-495-7440/7244/7444 (for emergency use only)

SUPERNOVAE 2003ag, 2003ah, AND 2003ai
     Further to IAUC 8064, B. Swift, M. Ganeshalingam, and W. Li
report the LOTOSS discovery of three apparent supernovae on
unfiltered KAIT images:

SN      2003 UT       R.A.  (2000.0)  Decl.   Mag.      Offset
2003ag  Feb. 7.5    11 26 01.82  + 1 59 02.8  16.5   12".5 E, 0".3 N
2003ah  Feb. 8.2     4 43 08.54  + 0 46 00.4  17.3   7".1 W, 7".0 N
2003ai  Feb. 8.5    13 00 58.68  +39 51 24.5  17.0   0".9 E, 7".7 S

Further approximate magnitude estimates:  SN 2003ag in UGC 6440,
2002 Dec. 27.4 UT, [19.0; 2003 Feb. 8.3, 16.3.  SN 2003ah, Jan.
29.2, [18.5; Feb. 9.2, 17.0.  SN 2003ai in IC 4062, 2002 June 16.3,
[19.0; 2003 Feb. 9.3, 16.9.

     On behalf of a large collaborative team, K. V. Getman, E. D.
Feigelson, and G. Garmire, Pennsylvania State University; and S. S.
Murray and F. R. Harnden, Jr., Smithsonian Astrophysical
Observatory, report the detection of an x-ray flare from the radio-
flaring object reported on IAUC 8055 and 8060, as seen with the
Chandra X-ray Observatory (+ ACIS-I detector) during an ultradeep
observation of the Orion nebula during Jan. 8-22.  The x-ray
variability has a complex morphology:  it is approximately constant
around 0.04 counts/s from Jan. 8.9 to 16.3 UT, rapidly rising to
0.19 counts/s starting Jan. 16.3, falling to 0.11 counts/s by Jan.
16.7 (where it remained constant for a day), rising to 0.35
counts/s and higher over several hours starting Jan. 17.7, falling
to 0.2 counts/s over one day (and remaining at that level for a
half day), rising again to 0.35 counts/s and higher starting Jan.
19.7, and falling to 0.2 counts/s over one day by the end of the
observation.  Preliminary spectral analysis confirms the previous
Chandra findings (Feigelson et al. 2002, Ap.J. 574, 258) that the
source is deeply embedded in a molecular cloud with a column
density of log N_H about 22.6 cm**-2 and with absorption-corrected
luminosities of log L_x about 31.3 and about 32.0 erg/s, for the
quiescent and flaring phases, respectively.  As this source does
not have a near-infrared excess (Muench et al. 2002, Ap.J. 573,
366), it may be an extreme example of a magnetically active weak-
line T-Tau star, such as V773 Tau or DoAr 21 (cf. Feigelson and
Montmerle 1985, Ap.J. 289, L19), rather than a rare radio flaring
protostar (e.g., IRS 5 near R CrA; cf. Taylor and Storey 1984,
MNRAS 209, 5P).

                      (C) Copyright 2003 CBAT
2003 February 9                (8068)            Daniel W. E. Green

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