Homogeneous Photometry for Star Clusters and Resolved Galaxies. II. Photometric Standard Stars

By P. Stetson. 2000

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Stars appearing in CCD images obtained over 224 nights during the course of 69 observing runs have been calibrated to the Johnson/Kron‐Cousins BVRI photometric system defined by the equatorial standards of Landolt (1992, AJ, 104, 340). More than 15,000 stars suitable for use as photometric standards have been identified, where “suitable” means that the star has been observed five or more times during photometric conditions and has a standard error of the mean magnitude less than 0.02 mag in at least two of the four bandpasses, and shows no significant evidence of intrinsic variability. Many of these stars are in the same fields as Landolt’s equatorial standards or Graham’s (1982, PASP, 94, 244) southern E‐region standards but are considerably fainter. This enhances the value of those fields for the calibration of photometry obtained with large telescopes. Other standards have been defined in fields containing popular objects of astrophysical interest, such as star clusters and famous galaxies, extending Landolt‐system calibrators to declinations far from the equator and to stars of subsolar chemical abundances. I intend to continue to improve and enlarge this set of photometric standard stars as more observing runs are reduced. The full current database of photometric indices is being made freely available via a site on the World Wide Web or via direct request to the author. Although the contents of the database will evolve in detail, at any given time it should represent the largest sample of precise BVRI broadband photometric standards available anywhere.

Subfields: Astronomy and Astrophysics, Computational Mechanics

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Citations in the corpus

The ACS Survey of Galactic Globular Clusters. I. Overview and Clusters without Previous Hubble Space Telescope Photometry (2006, methodology): “Our fiducial sequences for M92 andNGC6752 are consistent with those presented byBrown et al. (2005) and with the ground-based data of Stetson (2000) in the VI passbands.”
Gaia Early Data Release 3 (2020, methodology): “To devise a selection criteria for C∗ we made use of the Stetson and Ivezic standards (Stetson 2000; Ivezić et al. 2007) to determine the C∗ scatter versus G magnitude using all the sources in the sample with G > 9 (to avoid problems with low number statistics at the bright end).”
WINGS: a WIde-field Nearby Galaxy-cluster Survey. I. Optical imaging (2005, background): “Nowadays there are two main sets of standard fields that, even if they not provide a complete coverage of the CCD mosaic, can be used satisfactorily for wide field photometry, namely the sample of Landolt (1992) and that of Stetson (2000).”
SN 2003du: 480 days in the life of a normal type Ia supernova (2007, methodology): “The final image ZP and its uncertainty are, respectively, the average of the individual ZPs 2 Available athttp://cadcwww.hia.nrc.ca/standards/ and as discussed by Stetson (2000) this photometry is essentiallyin the Landolt (1992) system.”
MULTIPLE STELLAR POPULATIONS IN 47 Tucanae (2011, methodology): “…of the Advanced Camera for Surveys (ACS/WFC) and the UVIS channel of Wide Field Camera 3 (WFC3/UVIS), while to study the spatial distribution of the populations we made use of U, B, V, and I ground-based photometry from the data base of 856 original and archival CCD images from Stetson (2000).”
Deviations from the Local Hubble Flow. I. The Tip of the Red Giant Branch as a Distance Indicator (2002, methodology): “The magnitude zero point, c1, was computed by using the above information and aperture photometry of both Landolt standard stars and the additional stars in Landolt fields recently calibrated to the standard system (Stetson 2000).”
Ground-based CCD astrometry with wide-field imagers - II. A star catalog for M 67: WFI@2.2 m MPG/ESO astrometry, FLAMES@VLT radial velocities (2008, methodology): “Initially, we transformed our instrumental magnitudes obtained in B,V, I filters into the standard Johnson Kron-Cousins magnitudes using standard stars from Stetson’s1 secondary standard star catalog (Stetson 2000, 2005).”
GLOBULAR CLUSTERS IN THE OUTER GALACTIC HALO: NEW HUBBLE SPACE TELESCOPE/ADVANCED CAMERA FOR SURVEYS IMAGING OF SIX GLOBULAR CLUSTERS AND THE GALACTIC GLOBULAR CLUSTER AGE–METALLICITY RELATION (2011, methodology): “For the ∼20 stars that appear in both catalogs, the average offsets are less than 0.01 mag in V and I; the WFPC2 data were adjusted to match the photometric zeropoints of the standard stars measured by Stetson (2000).”
Complexity on Small Scales: The Metallicity Distribution of the Carina Dwarf Spheroidal Galaxy (2005, methodology): “Conveniently, the observed EIS fields overlap with a standard star field in Carina (Stetson 2000) allowing a direct comparison between the EIS-photometry and that provided by Stetson.”
Distance to the Large Magellanic Cloud: The RR Lyrae Stars (2003, methodology): “They are based on 127 measurements in two separate nights of 27 standard stars selected from Landolt (1992) - Stetson (2000) standard fields PG0918+029, PG0231+051, PG1047+003, and SA98, with magnitude and colors in the ranges 12.773 V 17.729, −0.273 B − V 1.936, −0.304 V − I 2.142.”
The SUMO project: a SUrvey of Multiple pOpulations in globular clusters (2013, methodology): “The new data were used to complement the extensive data base maintained by one of us (P.B. Stetson, see Stetson 2000), andin par- ticular to add the images in theU-band for a large number of clusters.”
Abundances in a Large Sample of Stars in M3 and M13 (2004, methodology): “Open circles denote those sample stars without I photometry from the database of Stetson (2000).”
Cepheid Distances to SNe Ia Host Galaxies Based on a Revised Photometric Zero Point of the HST WFPC2 and New PL Relations and Metallicity Corrections (2006, methodology): “…comparison of CTE corrected aperture photometry [according to prescription (Dolphin 2002), which is suitable for direct 0B5 aperture photometry] versus the ground-based sequences in NGC 2419 of Stetson (2000)5 and an early (before publication) version of the ground-based NGC 2419 sequence in SDTW.”
MULTI-ELEMENT ABUNDANCE MEASUREMENTS FROM MEDIUM-RESOLUTION SPECTRA. II. CATALOG OF STARS IN MILKY WAY DWARF SATELLITE GALAXIES (2010, background): “Stetson (2000) has made photometry publicly available for all of these clusters as part of his photometric standard field database.11 Every star has been measured in at least two of the Johnson-Cousins B, V , R, and I filters.”
Analysis and calibration of CaII triplet spectroscopy of red giant branch stars from VLT/FLAMES observations (2007, background): “The photometry and astrometry are from Stetson (2000).”
Empirical color transformations between SDSS photometry and Other photometric systems. (2005, methodology): “The problem of the reduced number of stars in common between the Landolt catalog and the SDSS due to saturation is alleviated by the extension of Landolt’s standard stars to fainter magnitudes by Stetson (2000).”
The Hα surface brightness–radius relation: a robust statistical distance indicator for planetary nebulae (2015, methodology): “The cluster distance of 3.0 kpc is derived from the reddening and distance modulus given by Mermilliod et al. (2001), in turn based on a deep colour-magnitude diagram from Stetson (2000).”