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[vsolj-alert 856] VSNET Weekly Campaign Summary

From owner-vsnet-campaign@kusastro.kyoto-u.ac.jp Tue Jan 30 05:28 JST 2001
To: vsnet-campaign
Date: Tue, 30 Jan 2001 05:28:06 +0900
From: Makoto Uemura <uemura@kusastro.kyoto-u.ac.jp>
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Subject: [vsnet-campaign 724] VSNET Weekly Campaign Summary
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VSNET Weekly Campaign Summary
*** Last week news ***

(new targets)
  SN 2001M		(RA = 10h24m31s.48, Dec = -21d47'40".6)

    SN 2001M was discovered and confirmed on Jan. 21.4 UT (mag 175:C) 
  and Jan. 22.4 UT (mag 177:C), respectingly.  The location is about 
  12" east and 12" south of the nucleus of a face-on spiral (SAB(rs)b) 
  galaxy NGC 3240.  This galaxy has a bright nucleus, but the new 
  object is well outside of the central region and embedded on the 
  outer disk.  There is mag 14 foreground star whose offsets from 
  the nucleus of NGC 3240 are about 22" east and 42" south.  
  The recession velocity of the host galaxy (3584 km/s) suggests that 
  expected maximum of a normal SN Ia would be mag 15.1 
  (vsnet-campaign-sn 139).

  SN 2001N		(R.A. = 10h39m58s.08, Dec = +24d05'26".0)

    SN 2001N was discovered and confirmed on Jan. 21.4 UT (mag 163:C)
  and Jan. 22.4 UT (mag 162:C), respectingly.  The location is very 
  close (3" SE) of the bright nucleus of a face-on spiral (SA(r)b) 
  galaxy NGC 3327.  There are some foreground stars: a mag 14 star 
  (GSC 1977-815, GSCmag(close to V)=14.09, USNO r=14.6, b=16.4 about 
  24" west of the nucleus of NGC 3327, and a mag 17: star (USNO_A2.0 
  position is end figures 57s.26, 57".6, r=17.1, b=17.6) about 9" west 
  and 29" north of the nucleus.  The recession velocity of the host 
  galaxy is 6303 km/s, so SN 2001N is now about as bright as the maximum 
  of a normal SN Ia (vsnet-campaign-sn 139).  

  MKN 421		(RA = 11h04m27s, Dec = +38d12'32")

    H.G. Boerst (University of Kiel), N. Goetting (University of Hamburg),
  and R. Remillard,(MIT) reported; following the detection of enhanced 
  X-ray emission from the BL Lac object Markarian 421 with the RXTE/ASM, 
  observations with the Cherenkov telescopes of HEGRA show very strong 
  TeV activity. Above a threshold energy of 500 GeV, daily integrated 
  fluxes (20 minute averages) reach up to 1, 4, 2, 1.5, 2.5, and 
  3 times the TeV flux of the Crab Nebula in consecutive nights during 
  January 16-22. The ASM observations of Mkn 421 in mCrab at 2-12 keV: 
  44(2) over UT 2001 January 13-18; 30(3) Jan 19-20; 54(3) on Jan 21, 
  and 80(6) on Jan 22.  The peak is the brightest X-ray flux seen 
  from a BL Lac object during the RXTE Mission (vsnet-campaign-blazar 128, 
  129, 134, vsnet-campaign-xray 60).  L. Takalo and R. Rekola reported 
  they have taken observations on Jan. 22 in B, V and R bands and 
  will take some additional data (vsnet-campaign-blazar 130).
  No exceedingly brightening at optical range has been observed to VSNET 
  (vsnet-campaign-blazar 133, 137), but observations on January 28 indicate 
  a possible one (vsnet-campaign-blazar 139).

  QW Ser		(RA = 15h26m13s.99, Dec = +08d18'03".8)

    P. Schmeer reported an outburst at 13.2mag of the SU UMa-type 
  dwarf nova QW Ser (=TmzV46) on January 25.  The most recently 
  observed outburst (a supermaximum) was detected by me on 2000 
  July 5.941 UT at mv= 12.4 (cf. vsnet-alert 5068).   Prior to that one 
  P. Schmeer had found three other outbursts: 1999 Oct. 4 (supermaximum), 
  2000 Jan. 4 (normal), May 1 (normal) (vsnet-campaign 714, 
  vsnet-campaign-dn 415).  It was faded to 13.7mag on January 26 as 
  reported by E. Muyllaert (vsnet-campaign-dn 418).  

  SX LMi		(RA = 10h54m29s.93, Dec = +30d06'30".0)
    As reported by M. Simonsen, the SU UMa-type dwarf nova SX LMi was 
  reported to be in outburst.  The present outburst is a relatively 
  bright one, suggesting a superoutburst.  The last superoutburst was 
  observed in 2000 March - April (cf. vsnet-alert 4492, 4496, 4499).
  (vsnet-campaign 715, vsnet-campaign-dn 416).
  The outburst is now continuing (vsnet-campaign-dn 419, 424).  

  3C 273		(RA = 12h29m6s.7, Dec = 02d03m08s)

    The famous quasar 3C 273 is reported bright (12.4mag on January 1 by 
  H. Maehara; 12.3mag on January 25 by M. Simonsen).  The object is the
  brightest in recent years (vsnet-campaign-blazar 135).

  BF Eri		(RA = 04h39m29s.62, Dec = -04d36'10".0)

    An outburst of the dwarf nova BF Eri was reported by M. Simonsen 
  on January 26 at 13.5mag.  The last outburst was observed in 2000 
  November - December (vsnet-campaign-dn 417).  The outburst continues 
  (vsnet-campaign-dn 428), and further brighter on January 28 
  (vsnet-campaign-dn 435).

  RX J0640-24		(RA = 06h40m47s.72, Dec = -24d23'14".5)

    As reported by R. Stubbings and B. Monard on January 26, 
  the potential SU UMa-type dwarf nova RX J0640-24 entered in an 
  outburst (12.4, 12.2mag).  The peak brightness was comparable 
  to those of short outbursts observed in the past (vsnet-campaign 716).
  The object faded on January as indicated by observations after January 
  27 (vsnet-campaign-dn 425, 433).

  U Gem			(RA = 07h55m05s.55, Dec = +22d00'09".2)

    Serveral observers reports that U Gem is brighter than usual 
  quiescence on January 27-28 (13.8mag; vsnet-campaign 717, 
  vsnet-campaign-dn 426, 430).  The slightly bright state at about 13.8 
  continues on January 29 (vsnet-campaign-dn 436).

  OJ 287		(RA = 08h51m57s, Dec = 20d17'59")

    The object is reported to be slightly fainter 
  (vsnet-campaign-blazar 138).

  V342 Cen		(RA = 11h07m15s.82, Dec = -55d57'32".7)

    As reported by R. Stubbings,  V342 Cen is now the first time 
  visually recorded in outburst (14.4mag on January 28).  
  R. Stubbings commented that the position agrees more with 
  the ROSAT  ID. (11h07 15.4  -55 57' 40") and it's interesting 
  to see that no star is shown on the DSS images but present on 
  the USNO-A2.0 data, which indicates a large-amplitude dwarf 
  nova (amplitude exceeding 6 mag?) or other kind of CV with large 
  light variation (vsnet-campaign 720).  The outburst continues on 
  January 29 (14.6mag; vsnet-campaign-dn 437).

  NSV06160		(RA =13h13m12s, Dec = -36d44'.4)

    As indicated by B. Monard's observations, the symbiotic variable 
  NSV06160, which had been in outburst since 2000 July, is reported 
  to be undergoing a rapid fading (11.5mag on January 28).  
  This fading may represent an eclipse (vsnet-campaign 721).

  RZ LMi		(RA = 09h51m50s.10, Dec = +34d07'29".8)

    Observations by M. Simonsen on January 25 show it entered a 
  superoutburst, which continues now (vsnet-campaign-dn 431). 
  J. Kemp noticed the campaign of this object will be performed 
  on April 2001 (see below "Future Schedule" or, vsnet-campaign 718, 
  vsnet-campaign-dn 429). 

  RZ Psc		(RA = 01h09m40s.07, Dec = +27d57'28".0)

    P. Schmeer reported RZ Psc is fading to 13.2mag on January 28.
  Most of the time RZ Psc stays at a maximum brightness of mv= 11.7.
  Since the record of reported fadings shows all events were short, 
  quick follow-up observations are necessary (vsnet-campaign 723).

(continuous targets)
  RX J1155.4-5641	(RA = 11h55m27s.03, Dec = -56d41'53".3)

    The bright outburst continues (vsnet-campaign 712, vsnet-campaign-dn 420, 
  vsnet-campaign-dn 427, 432).  The long outburst apparently entered 
  the rapid decline stage on January 29 as indicated by R. Stubbings 
  observation of 13.2mag (vsnet-campaign-dn 438).

  AG Hya		(RA = 09h50m30s.94, Dec = -23d45'03".7)

    The long outburst continued (vsnet-campaign-dn 412) until 
  January 26 when R. Stubbings reported the magnitudes of 15.1mag 
  indicating it started fading (vsnet-campaign-dn 421).

  SN 2001G		(RA = 09h09m33s.18, Dec = +50d16'51".3)

    The object seems to be keep at the maximum.  M. Reszelski reported 
  15.2mag on January 27 (vsnet-campaign-sn 140).

  V344 Ori		(RA = 06h15m18.94, Dec = +15d30'59".9)

    From M. Moilanen's CCD images taken on January 20, M. Uemura 
  estimates B-V=0.271 and V-R=0.246 of V344 Ori using Henden's sequence.
  In the light curve on January 22/23 by B. Martin, we can see two 
  maxima whose interval is about 3 - 4 hours, and shorter time-scale 
  modulations are also seen (vsnet-campaign-dn 414).  M. Uemura, 
  the Kyoto team, reported the object entered a rapid decline phase on 
  January 24 (vsnet-campaign 713).  Observations reported to VSNET 
  after January 23 confirms it (vsnet-campaign-dn 423).

  V445 Pup		(RA = 07h37m56s.88, Dec = -25d56'59".1)

    The object is relatively calm during the last week (vsnet-campaign-nova 
  187, 190, 191, 192, 193, 194, 195).  The discussions about the helium 
  nova scenario for V445 Pup are seen in [vsnet-campaign-nova 188, 189].

  TV Col		(RA = 05h29m25s.5, Dec = -32d49'05".2)

    Another very short outburst (12.8mag) occurred on January 28 
  as reported by R. Stubbings (vsnet-campaign-ip 37, 38).

  3C 66A		(RA = 02h22m39s.6, Dec = +43d02'08")

    The fading continues (vsnet-campaign-blazar 136).

  Delta Sco		(RA = 16h00m19s.9, Dec = -22d37'17")

    The observations since January 23 may indicate it is slightly 
  brighter (vsnet-campaign-be 81, 82).

  V803 Cen		(RA = 13h23m44.5s, Dec = -41d44'30".1)

    The fading from the outburst was observed on January 22 by B. Monard 
  (vsnet-campaign-dn 413), The object seems to recover the bright state 
  (vsnet-campaign-dn 422), and then, marked short-term variation on 
  January 28 (vsnet-campaign-dn 434).

*** Future schedule ***

  RZ LMi campaign conducted by J. Patterson on April 2001

    J. Kemp forwarded an invitation of RZ LMi campaign conducted by 
  J. Patterson on April 2001:
  "Since the work of Robertson et al. 1995 (PASP 107, 443) and Nogami et
   al. 1995 (PASJ 47, 897), this star has been known to be the most frantic
   dwarf nova in the sky, with superoutbursts popping off every 20
   days.  Five years ago we conducted a long CBA campaign, and found two
   tantalizing results: that the superhumps did not die in quiescence (as
   required by law), and that they did not lose track of phase from one
   superoutburst to the next (as required by another law).  The data were 
   not, however, sufficient to prove either of these beyond doubt."
    Time-series observations, especially longer than 3 hours, will 
  be welcomed.  For more general information about observations, 
  see "http://cba.phys.columbia.edu"; and click on "data" and "charts".  
  If you are interested in this campaign, please contact with J. Patterson 
				[vsnet-campaign 718, vsnet-campaign-dn 429]

*** General information ***

  MKN 421
    Comparison stars for observations: see [vsnet-campaign-blazar 131]
    Sequence by B. Skiff: see [vsnet-campaign-blazar 132]

  U Gem
    Eclipse ephemeris: see [vsnet-campaign 717]

  RX J2315.5-3049
    The result will be published as IBVS No. 5023.  The preprint is available
  as [vsnet-preprint 14].


						[vsnet-campaign 719]

(This summary is reproduction free.)

Makoto Uemura

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