J/AJ/124/3255       UBV photometry in M15                 (van der Marel+, 2002)
The following files can be converted to FITS (extension .fit .fgz or .fiZ)
Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/AJ/124/3255

drwxr-xr-x 38 cats archive 4096 Jan 29 2012 [Up] drwxr-xr-x 2 cats archive 4096 Dec 15 2013 [TAR file] -rw-r--r-- 1 cats archive 469 May 26 2013 .message -r--r--r-- 1 cats archive 4114 May 26 2013 ReadMe -rw-r--r-- 1 cats archive 1005 May 26 2013 +footg5.gif -rw-r--r-- 1 cats archive 2903 May 26 2013 +footg8.gif -r--r--r-- 1 cats archive 510504 Feb 10 2003 table1.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/AJ/124/3255 UBV photometry in M15 (van der Marel+, 2002) ================================================================================ Hubble Space Telescope evidence for an intermediate-mass black hole in the globular cluster M15. I. STIS spectroscopy and WFPC2 photometry. van der Marel R.P., Gerssen J., Guhathakurta P., Peterson R.C., Gebhardt K. <Astron. J. 124, 3255 (2002)> =2002AJ....124.3255V ================================================================================ ADC_Keywords: Clusters, globular ; Photometry, UBV Keywords: globular clusters: individual (M15) - stars: kinematics Abstract: In this series of two papers, we describe a project with the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope (HST) to measure the line-of-sight velocities of stars in the central few arcseconds of the dense globular cluster M15. This first paper focuses on the observations and reduction of the data. We "scanned" the central region of M15 spectroscopically by consecutively placing the 0.1" HST/STIS slit at 18 adjacent positions. The spectral pixel size exceeds the velocity dispersion of M15. This puts the project at the limit of what is feasible with STIS, and exceedingly careful and complicated data reduction and analysis were required. Description: WFPC2 images of M15 were obtained on 1994 April 7 in the context of HST program GO-5324 (PI: Yanny). Results from these observations were reported in a study led by one of us (Guhathakurta et al., 1996AJ....111..267G, hereafter G96). Data were obtained using the filters F336W, F439W, and F555W, respectively, which correspond roughly to the Johnson U, B, and V bands.