[vsnet-alert 5920] BVRI sequence for N AQL 2001

["Bruce Sumner" <b.sumner@bom.gov.au>]

I have prepared a preliminary BVRI sequence for Nova Aquilae 2001 
from Arne's single night field photometry. The sequence closely 
follows that chosen by Bouma [vsnetalert 5917] but I have extended 
it to fainter magnitudes. These will be revised as additional 
photometry becomes available. As Arne noted the magnitudes are 
accurate to about +/-0.02 magnitude.

Bruce Sumner
-----------------------------
221  NOVA AQUILAE 2001   (N)   Range: 10.8p19.6B
     Position:   19 07 28.39  +11 44 46.0  (J2000, from .dat file)
     Magnitude:  V=13.337  BV=1.765       (Henden, single night)

ID     RA  (2000)   DEC       X    Y  N     V     BV    VR    RI 

1   19 07 23.9  +11 43 34   67  72  1  10.437  0.401  0.463  0.271
2   19 07 18.3  +11 49 02  148  256  1  11.052  0.576  0.332  0.356 
3   19 07 47.1  +11 43 28   275  78  1  11.523  1.001  0.545  0.519 
4   19 07 27.1  +11 42 17   19 149  1  12.221  1.010  0.577  0.592 
5   19 07 12.5  +11 42 33  234 133  1  12.498  0.735  0.412  0.440 
6   19 07 41.2  +11 46 03   187   77  1  13.127  1.010  0.577  0.592 
7   19 07 43.2  +11 42 19   217 147  1  13.667  1.035  0.623  0.663 
8   19 07 43.5  +11 46 17   222   91  1  13.774  1.030  0.613  0.669 
9   19 07 39.4  +11 49 25   161  279  1  13.990  1.005  0.620  0.702 
10  19 07 29.3  +11 41 46    14 180  1  14.157  0.937  0.557  0.564  
11  19 07 31.9  +11 43 35    52  71  1  14.413  1.002  0.577  0.601 
12  19 07 37.4  +11 47 06   132  140  1  14.608  1.083  0.676  0.696 
13  19 07 17.9  +11 43 55  155  51  1  15.078  1.023  0.591  0.622 
14  19 07 32.1  +11 44 56    54   10  1  15.366  1.307  0.723  0.720
15  19 07 28.4  +11 43 52     0  54  1  15.840  1.160  0.686  0.615
16  19 07 29.6  +11 44 07    17  39  1  16.836  1.542  0.913  0.923  
 
Notes:

1. This preliminary sequence is based on field photometry obtained by 
Arne Henden on the single night of 22 May 2001. Errors are expected 
to be of the order of +/0.02 magnitude.

2. I have attempted to use stars of similar colour in this sequence 
to help observers estimate the magnitude of this red nova. This 
explains why the sequence stars generally have a colour as close as 
possible to BV=1.0.

3. Star #1 is saturated. It does have a reliable Tycho2 magnitude of 
10.29+/0.04.

Bruce Sumner
23 May 2001

VSNET Home Page

Return to Daisaku Nogami

---

vsnet-adm@kusastro.kyoto-u.ac.jp