From: James Brown (Jim_at_Seti.Net)
Date: Thu Jun 05 2008 - 15:44:15 PDT
Humm. That sucker is coming at us at 6,710,000 Miles/hour.
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From: "LARRY KLAES" <ljk4_at_msn.com>
Sent: Thursday, June 05, 2008 12:04 PM
To: <hits_at_setileague.org>
Subject: Hits: FW: ATel 1561. ***Instant Email Notice***: Novae
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>>From: atel_at_astronomerstelegram.org
>>To: ljk4_at_msn.com
>>Subject: ATel 1561. ***Instant Email Notice***: Novae
>>Date: 5 Jun 2008 11:41:47 -0700
>>
>>***Instant Email Notice***: Novae
>>
>>------------------------------------------------------------------------------
>>------------------------------------------------------------------------------
>>The Astronomer's Telegram
>>http://www.astronomerstelegram.org
>>==============================================================================
>>ATEL #1561 ATEL #1561
>>
>>Title: XMM-Newton RGS observation of V2491 Cyg
>>Author: J.-U. Ness and S. Starrfield (Arizona State University), R.
>> Gonzalez and E. Kuulkers (ESAC), J.P. Osborne and K. Page (University
>> of Leicester), G. Schwarz and K.M.Vanlandingham (West Chester
>> University),
>> J.J. Drake (Smithsonian Astrophysical Observatory), M. Hernanz
>> (CSIC-IEEC),
>> A. Evans (Keele University), N. Gehrels (NASA-GSFC), J. Krautter
>> (Landessternwarte
>> Heidelberg), R.D. Gehrz and C. Woodward (University of Minnesota)
>>Queries: Jan-Uwe.Ness_at_asu.edu
>>Posted: 5 Jun 2008; 18:30 UT
>>Subjects: X-ray, Binaries, Cataclysmic Variables, Novae, Transients
>>
>>On 2008, May 20.6 (39.9 days after outburst) we obtained an XMM-Newton
>>observation of the recent nova V2491 Cyg during the supersoft source
>>(SSS) phase (Osborne et al. 2008, ATel #1542). The exposure time in
>>the Reflection Grating Spectrometers (RGS) was 39.2ksec, and the
>>average
>>count rate in the RGS1 is 13.1 counts per sec (c/s). The light curve
>>extracted from the RGS1 is highly variable. The initial count rate is
>>15c/s, and 10ks into the observation it drops to 2c.s. The count rate
>>then reaches a level of 23c/s about 20ks into the observation and
>>remains
>>at that level until the end of the observation. The spectrum is that
>>of a bright SSS (hot white dwarf atmosphere) with continuous emission
>>ranging from 15Å to 35Å and a peak at 23Å. We find broad absorption
>>lines
>>at 15.84Å (OVIII at 16Å), 18.44Å (OVII at 18.62Å), 18.69Å (OVIII at
>>18.97Å),
>>20.70Å (NVII at 20.9Å), 21.36Å (OVII at 21.6Å), 24.51Å (NVII at 24.78Å),
>>and 28.48Å (NVI at 28.78Å). Assuming the rest wavelengths given in
>>brackets the lines are blue shifted by 3000km/s. This agrees with the
>>high expansion velocities determined early in the outburst from optical
>>(Tomov et al. 2008, ATel #1475). We further identify extremely broad
>>emission lines from NeX at 12.13A and NeIX triplet at 13.45/13.55/13.7A
>>which are at their rest wavelengths. We also find a weak line at the
>>rest wavelength of MgXII at 8.42Å. These emission lines are broadened
>>by more than 3000km/s (FWHM). The deepest absorption lines originate
>>from oxygen and the strongest emission lines originate from neon, which
>>suggests that V2491 Cyg may be an ONe nova.
>>
>>------------------------------------------------------------------------------
>>Password Certification: Jan-Uwe Ness (Jan-Uwe.Ness_at_asu.edu)
>>http://www.astronomerstelegram.org/?read=1561
>>==============================================================================
>>
>>
>>==============================================================================
>>This is an automatically-generated notice. If you'd like to be removed
>>from the mailing list, please visit the The Astronomer's Telegram at
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>>
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This archive was generated by hypermail 2.1.6 : Thu Jun 05 2008 - 15:54:26 PDT