The missing bulge globular clusters in M31 - New optical candidates

Wirth, Allan; Smarr, Larry; Bruno, Tara

doi:10.1086/162969

Cited by 20 publications

(19 citation statements)

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“…These two infrared sources are slightly dimmer but have colors consistent with those of the 2MASS sources with globular cluster and X-ray counterparts. CXOM31 J004221.5+411419 lies within 0>3 of a globular cluster candidate (S5 15) identified by Wirth, Smarr, & Bruno (1985). It is likely the same object as the Xray source 2E 0039.6+4057 seen with Einstein.…”

Section: Globular Clusters and Infrared Sourcesmentioning

confidence: 76%

AChandraHigh Resolution Camera Observation of X‐Ray Point Sources in M31

Kaaret

2002

ApJ

161

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We present results from a 47 ks observation of the Andromeda galaxy, M31, using the High Resolution Camera of the Chandra X-Ray Observatory. We detect 142 point sources spanning 3 orders of magnitude in luminosity, from L X ¼ 2 Â 10 35 to 2 Â 10 38 ergs s À1 in the 0.1-10 keV band. The X-ray source location accuracy is better than 1 00 in the central regions of the galaxy. One source lies within 1>3 of SN 1885 but does not coincide with the UV absorption feature identified as the supernova remnant. However, there is an optical transient, which is likely an optical nova, at the location of the X-ray source. There is a weak source, L X $ 4 Â 10 36 ergs cm 2 s À1 , coincident with the nucleus of M31 and 14 sources coincident with globular clusters. Our observation has very high efficiency down to luminosities of 1:5 Â 10 36 ergs s À1 for sources within 5 0 of the nucleus. Comparing with a ROSAT observation made 11 yr earlier, we find that 0:46 AE 0:26 of the sources with L X > 5 Â 10 36 ergs s À1 are variable. We find no evidence for X-ray pulsars in this region, indicating that the population is likely dominated by low-mass X-ray binaries. The source density radial profile follows a power-law distribution with an exponent of 1:25 AE 0:10 and is inconsistent with the optical surface brightness profile. The X-ray point-source luminosity function is well fitted by a differential broken power law with a break at a luminosity of ð4:5 þ1:1 À2:2 Þ Â 10 37 ergs s À1 . The luminosity function is consistent with a model of an aging population of X-ray binaries.

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Section: Globular Clusters and Infrared Sourcesmentioning

confidence: 76%

AChandraHigh Resolution Camera Observation of X‐Ray Point Sources in M31

Kaaret

2002

ApJ

161

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“…This nova is spatially associated with the M31 globular cluster Bol 126 (Wirth et al 1985). In Figure 4, we clearly see a brightening of the globular cluster by about one magnitude on around 2010 October 10 (Julian Date: 2455480).…”

Section: M31 2010-10fmentioning

confidence: 85%

CLASSICAL NOVAE IN ANDROMEDA: LIGHT CURVES FROM THE PALOMAR TRANSIENT FACTORY ANDGALEX

Cao

Kasliwal

Neill

et al. 2012

ApJ

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We present optical light curves of 29 novae in M31 during the 2009 and 2010 observing seasons of the Palomar Transient Factory (PTF). The dynamic and rapid cadences in PTF monitoring of M31, from one day to ten minutes, provide excellent temporal coverage of nova light curves, enabling us to record the photometric evolution of M31 novae in unprecedented detail. We also detect eight of these novae in the near-ultraviolet (UV) band with the Galaxy Evolution Explorer (GALEX) satellite. Novae M31N 2009-10b and M31N 2010-11a show prominent UV emission peaking a few days prior to their optical maxima, possibly implying aspherical outbursts. Additionally, our blueshifted spectrum of the recent outburst of PT And (M31N 2010-12a) indicates that it is a recurrent nova in M31 and not a dwarf nova in the Milky Way as was previously assumed. Finally, we systematically searched for novae in all confirmed globular clusters (GCs) of M31 and found only M31N 2010-10f associated with Bol 126. The specific nova rate in the M31 GC system is thus about one per year, which is not enhanced relative to the rate outside the GC system.

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“…Two of the Kaaret-WeCAPP sources with 2MASS fluxes (WeCAPP_V8946 and WeCAPP_V10578) have no globular cluster (gc) counterpart Kaaret (2002). While V8946 coincides with a gc-candidate identified by Wirth, Smarr, & Bruno (1985), a gc-counterpart for WeCAPP_V10578 is completely unknown. Another two of the WeCAPP-Kaaret sources (V16322 and V10431) have been identified as optical novae showing supersoft X-ray emission (Pietsch et al 2005).…”

Section: Correlation With Other Cataloguesmentioning

confidence: 99%

The Wendelstein Calar Alto Pixellensing Project (WeCAPP): the M 31 variable star catalogue

Fliri¹,

Riffeser

Seitz³

et al. 2005

A&A

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In this paper we present the WeCAPP catalogue of variable stars found in the bulge of M 31. Observations in the WeCAPP microlensing survey (optical R and I bands) for a period of three years (2000)(2001)(2002)(2003) resulted in a database with unprecedented time coverage for an extragalactic variable star study. We detected 23781 variable sources in a 16.1 × 16.6 field centered on the nucleus of M 31. The catalogue of variable stars contains the positions, the periods, and the variation amplitudes in the R and I bands. We classified the variables according to their position in the R-band period-amplitude plane. Three groups can be distinguished; while the first two groups can be mainly associated with Cepheid-like variables (population I Cepheids in group I; type II Cepheids and RV Tauri stars in group II), the third one consists of Long Period Variables (LPVs). We detected 37 RV Tauri stars and 11 RV Tauri candidates, which makes this catalogue one of the largest collections of this class of stars to date. The classification scheme is supported by Fourier decomposition of the light curves. Our data shows a correlation of the low-order Fourier coefficients Φ 21 with Φ 31 for classical Cepheids, as well as for type II Cepheids and RV Tauri stars. Correlating our sample of variable stars with X-ray based catalogues of Kaaret (2002, ApJ, 578, 114) and Kong et al. (2002, ApJ, 577, 738) results in 23 and 31 coincidences, 8 and 12 of which are M 31 globular clusters. The number density of detected variables is clearly not symmetric, which has to be included in the calculations of the expected microlensing event rate towards M 31. This asymmetry is due to the enhanced extinction in the spiral arms superimposed on the bulge of M 31, which reduces the number of sources to about 60%, if compared to areas of equivalent bulge brightness without enhanced extinction present.

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The missing bulge globular clusters in M31 - New optical candidates

Cited by 20 publications

References 0 publications

AChandraHigh Resolution Camera Observation of X‐Ray Point Sources in M31

AChandraHigh Resolution Camera Observation of X‐Ray Point Sources in M31

CLASSICAL NOVAE IN ANDROMEDA: LIGHT CURVES FROM THE PALOMAR TRANSIENT FACTORY ANDGALEX

The Wendelstein Calar Alto Pixellensing Project (WeCAPP): the M 31 variable star catalogue

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