<i>Galaxy Evolution Explorer</i>
                    Ultraviolet Photometry of Globular Clusters in M31

Rey, Soo-Chang; Rich, R. Michael; Lee, Young-Wook; Yoon, Suk-Jin; Yi, Sukyoung K.; Bianchi, Luciana; Sohn, Young-Jong; Friedman, Peter G.; Barlow, Tom A.; Byun, Yong Ik; Donas, J.; Forster, Karl; Heckman, Timothy M.; Jee, M. James; Jelinsky, Patrick; Kim, Suk Whan; Lee, Jae Woo; Madore, Barry F.; Malina, Roger F.; Martin, D. Christopher; Milliard, B.; Morrissey, Patrick; Neff, Susan G.; Rhee, Jaehyon; Schiminovich, David; Siegmund, Oswald H. W.; Small, Todd; Szalay, Alexander S.; Welsh, Barry Y.; Wyder, Ted K.

doi:10.1086/422412

Cited by 19 publications

(17 citation statements)

References 34 publications

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“…There is large scatter at all metallicities and no strong trend with metallicity (although the UV sample is far from complete). Meanwhile, the recent GALEX observations by Rey et al (2005) show that the far-UV properties of M31 GCs are similar to those of Milky Way GCs. By contrast, the UV fractions among nearby galaxies in the IUE sample appear to increase strongly with metallicity.…”

Section: Hot Stars In Elliptical Galaxiesmentioning

confidence: 95%

Hot Populations in M87 Globular Clusters

et al. 2006

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We have obtained HST/STIS far- and near-UV photometry of globular clusters in four fields in the gE galaxy M87. To a limit of m(FUV) = 25 we detect a total of 66 globular clusters (GCs) in common with the deep HST optical-band study of Kundu et al. (1999). Despite strong overlap in V- and I-band properties, the M87 GCs have UV/optical properties that are distinct from clusters in the Milky Way and in M31. M87 clusters, especially metal-poor ones, produce larger hot HB populations than do Milky Way analogues. Cluster mass is probably not a factor in these distinctions. The most metal-rich M87 GCs in our sample are near Z_sun and overlap the local E galaxy sample in estimated Mg_2 line indices. Nonetheless, the clusters produce much more UV light at a given Mg_2, being up to 1 mag bluer than any gE galaxy in (FUV-V) color. The M87 GCs do not appear to represent a transition between Milky Way-type clusters and E galaxies. The differences are in the correct sense if the clusters are significantly older than the E galaxies. Comparisons with Galactic open clusters indicate that the hot stars lie on the extreme horizontal branch, rather than being blue stragglers, and that the EHB becomes well populated for ages > 5 Gyr. We find that 43 of our UV detections have no optical-band counterparts. Most appear to be UV-bright background galaxies, seen through M87. Eleven NUV variable sources detected at only one epoch in the central field are probably classical novae. [Abridged]Comment: 70 pages, 25 figures (including 4 jpgs), 7 tables. To appear in AJ. Full resolution version available at http://www.astro.virginia.edu/~rwo/m87/m87-hotpops.pd

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Section: Hot Stars In Elliptical Galaxiesmentioning

confidence: 95%

Hot Populations in M87 Globular Clusters

et al. 2006

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“…A total of 23 images (about 17 deg 2 ) have covered most of the disk and halo of M31. The details of the GALEX observations for M31 are presented in Rey et al (2005Rey et al ( , 2007.…”

Section: Galex Ultraviolet Datamentioning

confidence: 99%

A COMPREHENSIVE GALEX ULTRAVIOLET CATALOG OF STAR CLUSTERS IN M31 AND A STUDY OF THE YOUNG CLUSTERS

Kang¹,

Rey²,

Bianchi³

et al. 2012

ApJS

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We present a comprehensive catalog of 700 confirmed star clusters in the field of M31 compiled from three major existing catalogs. We detect 418 and 257 star clusters in Galaxy Evolution Explorer near-ultraviolet and far-ultraviolet (FUV) imaging, respectively. Our final catalog includes photometry of star clusters in up to 16 passbands ranging from FUV to NIR as well as ancillary information such as reddening, metallicity, and radial velocities. In particular, this is the most extensive and updated catalog of UV-integrated photometry for M31 star clusters. Ages and masses of star clusters are derived by fitting the multi-band photometry with model spectral energy distribution (SED); UV photometry enables more accurate age estimation of young clusters. Our catalog includes 182 young clusters with ages less than 1 Gyr. Our estimated ages and masses of young clusters are in good agreement with previously determined values in the literature. The mean age and mass of young clusters are about 300 Myr and 10 4 M , respectively. We found that the compiled [Fe/H] values of young clusters included in our catalog are systematically lower (by more than 1 dex) than those from recent high-quality spectroscopic data and our SED-fitting result. We confirm that most of the young clusters' kinematics shows systematic rotation around the minor axis and association with the thin disk of M31. The young cluster distribution exhibits a distinct peak in the M31 disk around 10-12 kpc from the center and follows a spatial distributions similar to other tracers of disk structure such as OB stars, UV star-forming regions, and dust. Some young clusters also show concentration around the ring splitting regions found in the southern part of the M31 disk and most of them have systematically younger (<100 Myr) ages. Considering the kinematical properties and spatial distribution of young clusters, they might be associated with the well-known 10 kpc star formation ring structure in the M31 disk. Consequently, we suggest that various properties of young clusters in M31 might be in line with the scenarios that a satellite galaxy had passed through the disk of M31 less than few hundred million years ago.

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“…We performed aperture photometry using the APPHOT package in IRAF, 7 with a 6 pixel aperture for the photometry (see Rey et al 2005), and we calculated an aperture correction examining isolated stars. We converted the observed count rates to fluxes and AB magnitudes using conversion factors outlined in the GALEX observers handbook.…”

Section: Uv and Optical Imagesmentioning

confidence: 99%

A Census of the Supersoft X-Ray Sources in M31

Orio¹,

Nelson²,

Bianchini³

et al. 2010

ApJ

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We examined X-ray, ultraviolet, and optical archival data of 89 supersoft X-ray sources (SSS) in M31. We studied the timescales of X-ray variability and searched UV and optical counterparts. Almost a third of the SSS are known classical or recurrent novae, and at least half of the others exhibit the same temporal behavior as post-outburst novae. Non-stellar objects among SSS seem to be rare: less than 10% of the classified SSS turned out to be supernova remnants, and only one source has been identified with an active galactic nucleus in the background. Not more than 20% of the SSS that are not coincident with observed novae are persistent or recurrent X-ray sources. A few of these long-lasting sources show characteristics in common with other SSS identified as white dwarf (WD) close binaries in the Magellanic Clouds and in the Galaxy, including variability on timescales of minutes, possibly indicating the spin period of a WD. Such objects are likely to be low-mass X-ray binaries with a massive WD. A third of the non-nova SSS are in regions of recent star formation, often at the position of an O or B star, and we suggest that they may be high-mass X-ray binaries. If these sources host a massive hydrogen-burning WD, as it seems likely, they may become Type Ia supernovae (SNe Ia), constituting the star formation dependent component of the SNe Ia rate.

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Galaxy Evolution Explorer Ultraviolet Photometry of Globular Clusters in M31

Cited by 19 publications

References 34 publications

Hot Populations in M87 Globular Clusters

Hot Populations in M87 Globular Clusters

A COMPREHENSIVE GALEX ULTRAVIOLET CATALOG OF STAR CLUSTERS IN M31 AND A STUDY OF THE YOUNG CLUSTERS

A Census of the Supersoft X-Ray Sources in M31

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