J/A+A/439/433 RIJ photometry of stars around PSR B1718-19 (Janssen+, 2005)
Observations of the binary pulsar system PSR B1718-19.
The role of tidal circularization.
Janssen T., Van Kerkwijk M.H.
<Astron. Astrophys. 439, 433 (2005)>
=2005A&A...439..433J 2005A&A...439..433J
ADC_Keywords: Pulsars ; Binaries, eclipsing ; Photometry, infrared
Keywords: binaries: eclipsing - pulsars: individual (PSR B1718-19) -
stellar dynamics
Description:
In our paper we present VLT-observations in R, I and J of the
candidate companion of PSR B1718-19, and also make use of HST
observations in F702W, previously presented in Van Kerkwijk et al.,
2000ApJ...529..428V 2000ApJ...529..428V. We make available online our astrometry and
photometry including error-bars. The field-size is approximately 34x34
arcsec (F702W), 80x80 arcsec (R & I), and 89x89 arcsec (J).
Objects:
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RA (2000) DE Designation(s)
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17 21 01.5 -19 36 51 PSR B1718-19 = EQ J1721-1936
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 97 2390 Positions and apparent magnitudes of the candidate
companion of PSR B1718-19 and surrounding stars
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- Seq Star label
7- 20 F14.10 deg RAdeg Right ascension (J2000) (1)
23- 36 F14.10 deg DEdeg Declination (J2000) (1)
39- 47 F9.3 mag Rmag ?=0.000 Apparent magnitude in R (657nm) (2)
49- 57 F9.3 mag e_Rmag ?=0.000 Sigma of apparent magnitude in R (3)
59- 67 F9.3 mag Imag ?=0.000 Apparent magnitude in I (768nm) (2)
69- 77 F9.3 mag e_Imag ?=0.000 Sigma of apparent magnitude in I (3)
79- 87 F9.3 mag Jmag ?=0.000 Apparent magnitude in J (1.25um) (2)
89- 97 F9.3 mag e_Jmag ?=0.000 Sigma of apparent magnitude in J (3)
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Note (1): The uncertainty in the zero-point of the astrometry is 0.06arcsec
(see Van Kerkwijk et al., 2000ApJ...529..428V 2000ApJ...529..428V). For this table only
the HST/F702W-astrometry has been corrected for field distortion,
using the standard correction of HSTPhot.
For VLT/FORS-bands R & I the distortion is small (smaller than
∼0.15arcsec), as the astrometry and photometry is done on a subframe
measuring 400x400 pixels (out of a total of 2048x2048 pixels).
For VLT/ISAAC-band J the distortion is larger (amounting up to
∼0.3arcsec at the edges of the subframe). Consequently, the
uncertainty in the astrometry is expected to be lowest in F702W,
intermediate in R & I, and highest in J.
The astrometry listed in this table has therefore been done in one of
the filters F702W, I, R, or J (in that order) if a detection occurred
in that filter.
Note (2): Value 0.000 means no detection or cross-identification
occurred in that filter.
Note (3): The uncertainty in the photometric zero-point is 0.02 (J)
or smaller than 0.03 (R & I). These uncertainties have not been
added to the error-bars listed in this table.
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Acknowledgements: T. Janssen, T.Janssen(at)phys.uu.nl
References:
Van Kerkwijk et al., Paper I 2000ApJ...529..428V 2000ApJ...529..428V
(End) Patricia Vannier [CDS] 05-Apr-2005