The progenitor of Nova Monocerotis 2012
ATel #4365; R. Greimel (U. Graz), J. Drew (U. Hertfordshire), D. Steeghs (U. Warwick), M. Barlow (UCL) on behalf of the IPHAS collaboration
on 10 Sep 2012; 11:49 UT
Credential Certification: Danny Steeghs (email@example.com)
Subjects: Infra-Red, Optical, Binary, Cataclysmic Variable, Nova, Transient
We report on the detection of the likely progenitor to Nova Mon 2012
using images from the INT Photometric H-Alpha Survey (IPHAS; http://www.iphas.org ). Nova Mon 2012 was discovered in the optical on August 9
(CBET #3202) and was recently found to be coincident with the gamma-ray
transient Fermi J0639+0548 (ATel #4224, ATel #4310). Follow up observations
of the Nova in the optical (ATel #4320),UV and X-Ray (Atel #4321) and radio (ATel #4352)
were also recently reported.
The fields containing the classical nova were observed as part of our galactic
plane survey using the Wide Field Camera (0.33"/pixel) at the 2.5m Isaac Newton
Telescope. Seeing was stable around 1.1" for the observations which were
calibrated using standard stars taken on the same night and corrected by the
global survey calibration. The measurement are listed in the table below. Magnitudes
are on the Vega scale and magnitude errors are dominated by the external
global calibration error of 0.03 magnitudes.
Table of observations:
Date and Time(UT) Field r rerr i ierr Ha Haerr r-i r-Ha
2004 11 4.2490 3743 18.05 0.03 17.39 0.04 17.58 0.04 0.66 0.47
2004 11 4.2521 3743o 17.92 0.03 17.24 0.04 17.59 0.04 0.68 0.33
2004 11 6.2153 3757 17.78 0.03 17.06 0.03 17.24 0.03 0.72 0.54
A single point source was detected at the position of the nova.
The variability of the nova counterpart is 5 times larger than that of
surrounding stars. The r-Halpha colour index is about 0.5 and also shows variability.
The nova progenitor lies above the main locus of fields stars implying
mild Halpha line emission.
The IPHAS counterpart coincides with the UKIDSS (Lucas et al., 2008, MNRAS 391,
136)) source UGPS J069978.60+055332.9 at J=16.26, H=15.71 and K=15.42.
The next closest IPHAS point source is 6" away.
The total galactic extinction along the line of sight amounts to E(B-V)=0.8
(Schlafly & Finkbeiner 2011, ApJ 737, 103, dust-maps as well as our own field
star photometry), while outburst spectroscopy indicates E(B-V)=0.3
The IPHAS and UKIDSS colours are consistent with an early K SED reddened by
E(B-V)=0.3 with an Halpha EW of 10-15 A (see also Drew et al. 2005, MNRAS 362,
752). If instead an optically thick accretion disk SED is assumed, it would
require a reddening of E(B-V)=0.8, the maximum possible for this sightline, and
Halpha EW of 15-20 A to be consistent with the IPHAS colours.
The Isaac Newton Telescope is operated on the island of La Palma by the Isaac
Newton Group in the Spanish Observatorio del Roque de los Muchachos of the
Instituto de Astrofisica de Canarias
This research has made use of: the NASA/IPAC Extragalactic Database (NED) which
is operated by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration; the VizieR catalogue access tool, CDS, Strasbourg, France. The
original description of the VizieR service was published in A&AS 143, 23