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[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

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