2MASS NIR photometry for 693 candidate globular clusters  in M 31 
and the Revised Bologna Catalogue

Galleti, S.; Federici, L.; Bellazzini, M.; Pecci, F. Fusi; Macrina, S.

doi:10.1051/0004-6361:20035632

Cited by 224 publications

(442 citation statements)

References 33 publications

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“…We detected two new sources in the M 31 GCs Bol 111 and Bol 194 (Galleti et al 2004). For both sources follow-up ToO observations with the Swift X-ray Telescope (XRT) were requested (e.g.…”

Section: X-ray Observations and Data Analysismentioning

confidence: 99%

“…To obtain astrometrically-corrected positions we selected optical sources, with proper-motion corrected positions, from the USNO-B1.0 catalogue (Monet et al 2003), and checked that only one optical source was in the error circle of the corresponding X-ray source. We only accepted sources correlating with globular clusters from the Revised Bologna Catalogue (V.3.4, January 2008; Galleti et al 2004Galleti et al , 2005Galleti et al , 2006Galleti et al , 2007 or with foreground stars, characterized by their optical to X-ray flux ratio (Maccacaro et al 1988) and their hardness ratio (see Stiele et al 2008). We then used the XMMSAS task eposcorr to derive the offset of the X-ray aspect solution.…”

Section: X-ray Observations and Data Analysismentioning

confidence: 99%

“…There are about 500 GCs known that belong to M 31 (482 confirmed GCs, according to the Revised Bologna Catalogue 8 (V.3.5, March 2008; Galleti et al 2004Galleti et al , 2005Galleti et al , 2006Galleti et al , 2007). This corresponds approximately to a stellar mass of about 5 × 10 9 M .…”

Section: Globular Cluster Nova Rate -The Optical Point Of Viewmentioning

confidence: 99%

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The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae

Henze

Pietsch

Haberl

et al. 2009

A&A

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Context. Classical novae (CNe) have been found to represent the major class of supersoft X-ray sources (SSSs) in our neighbour galaxy M 31. Aims. We determine the properties and evolution of the two first SSSs ever discovered in the M 31 globular cluster (GC) system. Methods. We have used XMM-Newton, Chandra and Swift observations of the centre region of M 31 to discover both SSSs and to determine their X-ray light curves and spectra. We performed detailed analysis of XMM-Newton EPIC PN spectra of the source in Bol 111 (SS1) using blackbody and NLTE white dwarf (WD) atmosphere models. For the SSS in Bol 194 (SS2) we used optical monitoring data to search for an optical counterpart. Results. Both GC X-ray sources were classified as SSS. We identify SS1 with the CN M31N 2007-06b recently discovered in the M 31 GC Bol 111. For SS2 we did not find evidence for a recent nova outburst and can only provide useful constraints on the time of the outburst of a hypothetical nova. Conclusions. The only known CN in a M 31 GC can be identified with the first SSS found in a M 31 GC. We discuss the impact of our observations on the nova rate for the M 31 GC system.

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“…We detected two new sources in the M 31 GCs Bol 111 and Bol 194 (Galleti et al 2004). For both sources follow-up ToO observations with the Swift X-ray Telescope (XRT) were requested (e.g.…”

Section: X-ray Observations and Data Analysismentioning

confidence: 99%

Section: X-ray Observations and Data Analysismentioning

confidence: 99%

See 1 more Smart Citation

The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae

Henze

Pietsch

Haberl

et al. 2009

A&A

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“…All observational data for GCs was compiled using catalogs from the following references: Georgiev et al (2009a,b); Forbes & Bridges (2010); ; Strader et al (2011); Galleti et al (2004); Peacock et al (2010); Harris (1996Harris ( ) (2010 Edition. In addition, this work made use of catalogs from Ochsenbein et al (2000).…”

mentioning

confidence: 99%

Clues on the missing sources of reionization from self-consistent modelling of Milky Way and dwarf galaxy globular clusters

Katz¹,

Ricotti²

2014

Monthly Notices of the Royal Astronomical Society

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Globular clusters are unique tracers of ancient star formation. We determine the formation efficiencies of globular clusters across cosmic time by modeling the formation and dynamical evolution of the globular cluster population of a Milky Way type galaxy in hierarchical cosmology, using the merger tree from the Via Lactea II simulation. All of the models are constrained to reproduce the observed specific frequency and initial mass function of globular clusters in isolated dwarfs. Globular cluster orbits are then computed in a time varying gravitational potential after they are either accreted from a satellite halo or formed in situ, within the Milky Way halo.We find that the Galactocentric distances and metallicity distribution of globular clusters are very sensitive to the formation efficiencies of globular clusters as a function of redshift and halo mass. Our most accurate models reveal two distinct peaks in the globular cluster formation efficiency at z ∼ 2 and z ∼ 7 − 12 and prefer a formation efficiency that is mildly increasing with decreasing halo mass, the opposite of what expected for feedback-regulated star formation. This model accurately reproduces the positions, velocities, mass function, metallicity distribution, and age distribution of globular clusters in the Milky Way and predicts that ∼ 40% formed in situ, within the Milky Way halo, while the other ∼ 60% were accreted from about 20 satellite dwarf galaxies with v cir > 30 km/s, and about 29% or all globular clusters formed at redshifts z > 7.These results further strengthen the notion that globular cluster formation was an important mode of star formation in high-redshift galaxies and likely played a significant role in the reionization of the intergalactic medium.

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“…The sources were selected from the updated Revised Bologna Catalogue of M31 globular clusters and candidates (RBC v.4, available from http://www.bo.astro.it/M31; Galleti et al, 2004Galleti et al, , 2006Galleti et al, , 2007Galleti et al, , 2009, which is the latest and most comprehensive M31 GC catalogue so far. The catalogue contains 2045 objects, including 663 confirmed star clusters, 604 cluster candidates, and 778 other objects that were previously thought to be GCs but later proved to be stars, asterisms, galaxies, or HII regions.…”

Section: Sample Selectionmentioning

confidence: 99%

Spectroscopic study of globular clusters in the halo of M31 with the Xinglong 2.16 m telescope II: dynamics, metallicity and age

Zhang¹,

Huang²,

Li³

et al. 2012

Res. Astron. Astrophys.

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In our Paper I, we performed the spectroscopic observations of 11 confirmed GCs in M31 with the Xinglong 2.16m telescope and we mainly focus on the fits method and the metallicity gradient for the M31 GC sample. In this paper, we analyzed and discussed more about the dynamics, metallicity and age, and their distributions as well as the relationships between these parameters. In our work, eight more confirmed GCs in the halo of M31 were observed, most of which lack the spectroscopic information before. These star clusters are located far from the galactic center at a projected radius of ∼ 14 to ∼ 117 kpc, which are more spatially extended than that in the previous work. The Lick absorption-line indices and the radial velocities have been measured primarily. Then the ages, metallicities [Fe/H] and [α/Fe] have been fitted by comparing the observed spectral feature indices and the SSP model of Thomas et al. in the Cassisi and Padova stellar evolutionary tracks, respectively. Our results show that most of the star clusters of our sample are older than 10 Gyr except B290∼ 5.5 Gyr, and most of them are metal-poor with the metallicity [Fe/H] < −1, suggesting that these clusters were born at the early stage of the galaxy's formation. We find that the metallicity gradient for the outer halo clusters with r p > 25 kpc may not exist with a slope of −0.005 ± 0.005 dex kpc −1 and if the outliers G001 and H11 are excluded, the slope dose not change significantly with a value of −0.002 ± 0.003 dex kpc −1 . We also find that the metallicity is not a function of age for the GCs with age < 7 Gyr while for the old GCs with age > 7 Gyr there seems to be a trend that the older ones have lower metallicity. Besides, We plot metallicity distributions with the largest sample of M31 GCs so far and it shows the bimodality is not significant and the number of the metal-poor and metal-rich groups becomes comparable. The spatial distributions shows that the metal-rich group is more centrally concentrated while the metal-poor group is occupy a more extended halo and the young population is centrally concentrated while the old populaiton is more extended spatially to the outer halo.

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2MASS NIR photometry for 693 candidate globular clusters in M 31 and the Revised Bologna Catalogue

Cited by 224 publications

References 33 publications

The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae

The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae

Clues on the missing sources of reionization from self-consistent modelling of Milky Way and dwarf galaxy globular clusters

Spectroscopic study of globular clusters in the halo of M31 with the Xinglong 2.16 m telescope II: dynamics, metallicity and age

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