[Message Prev][Message Next][Thread Prev][Thread Next][Message Index][Thread Index]
[vsnet-campaign 265] (fwd) NY Ser
(fwd) NY Ser
From vsnet-alert 5045:
--------------------------------------------------------------------------
Date: Thu, 29 Jun 2000 02:00:44 +0200 (MET DST)
From: Daisaku Nogami <daisaku@uni-sw.gwdg.de>
Subject: [vsnet-alert 5045] NY Ser
Dear colleagues,
Our spectroscopic observations of NY Ser (= PG 1510+234)
at the Calar Alto Observatory are scheduled on the nights
of July 08/09 and 09/10. Because it is quite important
for us to know the state of NY Ser at our observations as
accurately as possible, we would ask observers to make a
close monitor of this star for ~1 month from now.
NY Ser is a quite interesting star, since this star is
considered to be the first SU UMa-type dwarf nova at the
midst of the period gap and causes outbursts frequently,
with a cycle of ~8 days (for more detail, see Nogami et al.
1998, PASJ 50, L1; Iida et al. 1995, IBVS No. 4208).
A finding chart is available via the chart archives of
VSNET:
GIF chart; http://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/charts/GIF/pg1510.gif
or
PG1510+234.ps under http://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/charts/.
Downes & Shara (1993, PASP 105, 127) also contains a finding
chart as Ser1.
I attach the photometric sequence of this star created by
Arne Henden and Bruce Sumner, which is available from the URL:
http://ftp.nofs.navy.mil/pub/outgoing/aah/sequence/sumner/nyser.seq
Thank you very much, Arne and Bruce!
Best regards,
Daisaku Nogami
-------------------------------------------------
145 NY SERPENTIS (UGSU) Range: 14.4-17.9V
Position: 15 13 02.32 +23 15 08.8 (J2000, from .dat file)
Magnitude: V=15.119 B-V=-0.002 (from .dat file)
ID RA (2000) DEC X Y N V ERR B-V ERR
a) Comparison star sequence
1 15 13 12.3 +23 18 37 138 208 3 13.744 0.006 0.911 0.006
2 15 12 39.9 +23 16 28 -309 79 3 13.799 0.006 0.553 0.005
3 15 13 18.8 +23 10 40 228 -269 3 14.042 0.011 0.838 0.004
4 15 12 37.6 +23 12 42 -340 -147 3 14.382 0.012 0.701 0.002
5 15 13 01.6 +23 21 29 -10 380 2 14.678 0.008 0.808 0.009
6 15 12 47.5 +23 13 07 -204 -122 3 15.532 0.009 0.830 0.005
7 15 12 58.9 +23 15 30 -47 21 3 15.885 0.009 0.577 0.002
8 15 13 23.9 +23 17 39 297 149 3 16.218 0.011 1.138 0.005
9 15 13 12.9 +23 11 48 146 -201 3 16.426 0.009 0.778 0.005
10 15 13 05.6 +23 12 33 45 -156 3 16.755 0.011 1.139 0.008
11 15 13 03.4 +23 17 27 15 138 3 17.510 0.018 0.676 0.026
12 15 13 08.2 +23 14 46 81 -24 3 17.873 0.013 0.700 0.021
13 15 13 06.4 +23 15 48 57 39 3 18.653 0.050 0.444 0.071
b) Wide-colour extension for CCD calibration
15 12 54.0 +23 17 49 -114 160 3 16.988 0.109 0.248 0.045
15 12 42.3 +23 10 45 -276 -264 3 18.151 0.062 0.437 0.268
15 13 13.3 +23 15 39 152 30 3 16.776 0.009 1.494 0.015
15 13 10.2 +23 12 14 109 -175 3 16.788 0.000 1.549 0.017
Notes:
The CBA chart for this variable has two comparison stars marked, namely
C1 and C2. One of these is included in the above sequence, and the other
is included in the wide-colour extension (it was too red to include in
the comparison star sequence). Details are as follows:
CBA Henden
V B-V
C1 15.885 0.577
C2 16.776 1.494
The bluest star in the wide-colour extension has a large error, and may
be a small amplitude variable. If used, it should be used with care.
The rounded visual magnitudes in this sequence are identical to those of
the preliminary one night sequence dated 21 June 1999.
Bruce Sumner
Revised 24 June 1999
vsnet-adm@kusastro.kyoto-u.ac.jp
Return to Daisaku Nogami
vsnet-adm@kusastro.kyoto-u.ac.jp
VSNET Home Page