Wide-field<i>HST</i>/ACS images of M81: the population of compact star clusters

Santiago-Cortés, M.; Mayya, Y. D.; Rosa-González, D.

doi:10.1111/j.1365-2966.2010.16531.x

Cited by 24 publications

(21 citation statements)

References 50 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Bends in SSC LFs have typically been found in the range of M ∼ −9 to −11 mag in V RI filters (e.g. Whitmore et al 1999;Gieles et al 2006a,b;Santiago-Cortés et al 2010;Adamo et al 2010Adamo et al , 2011a. Assuming typical un-extincted (and age dependent) optical-to-K-band colour indices of 2 to 3 mag, one would expect a corresponding bend to appear at MK ∼ −12 to −13 mag.…”

Section: Iras 18293-3413: What Could a Broken Power-law Reflect?mentioning

confidence: 99%

The K-band luminosity functions of super star clusters in luminous infrared galaxies, their slopes and the effects of blending

Randriamanakoto¹,

Vaïsänen²,

Ryder³

et al. 2013

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Super star clusters (SSCs) are typically found in interacting galaxies and trace an extreme form of star-formation. We present a K-band study of SSC candidates in a sample of local luminous infrared galaxies (LIRGs) using two adaptive optics instruments (VLT/NACO and Gemini/ALTAIR/NIRI). In addition to facilitating SSC detections in obscured environments, this work introduces SSC studies in hosts with higher star-formation rates (SFRs) than most previous studies. We find that the luminosity functions (LFs) of the clusters are reasonably well-fitted by a single power-law with the values of the index α ranging between 1.5 to 2.4 with an average value of α ≈ 1.9. This value appears to be less steep than the average α ≈ 2.2 in normal spiral galaxies. Due to the host galaxy distances involved (median D L ∼ 70 Mpc) blending effects have to be taken into account, and are investigated using Monte Carlo simulations of blending effects for LFs and a photometric SSC analysis of the wellstudied Antennae system which is artificially redshifted to distances of our sample. While blending tends to flatten LFs our analyses show that ∆α is less than ∼ 0.1 in our sample. The simulations also show that in the luminosity range, M K < −13, considered in this work the extracted SSC luminosities are generally dominated by a single dominant star cluster rather than several knots of SF. We present resolutionand distance-dependent SSC surface density confusion limits and show how blending rates and aperture sizes affect the LFs. The smallest possible apertures should be used in crowded regions.

show abstract

Section: Iras 18293-3413: What Could a Broken Power-law Reflect?mentioning

confidence: 99%

The K-band luminosity functions of super star clusters in luminous infrared galaxies, their slopes and the effects of blending

Randriamanakoto¹,

Vaïsänen²,

Ryder³

et al. 2013

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“… Sources: (1) This paper, (2) Lee et al (2008), (3) Verolme et al (2002), (4) Spitler et al (2008), (5) Gebhardt et al (2003), (6) Bassino et al (2006), (7) Dirsch et al (2003), (8) Gebhardt et al (2007), (9) Houghton et al (2006), (10) Gebhardt & Kissler‐Patig (1999), (11) Kundu & Whitmore (2001), (12) Harris & van den Bergh (1981), (13) Gebhardt et al (2000), (14) Giordano et al (2005), (15) Ferrarese, Ford & Jaffe (1996), (16) Peng et al (2008), (17) Bower et al (1998), (18) Shen & Gebhardt (2010), (19) Tamura et al (2006), (20) Macchato et al (1997), (21) Nowak et al (2007), (22) Gultekin et al (2009b), (23) Graham (2008), (24) Jordán A. et al (2005), (25) Harris (2010), (26) Cappellari et al (2009), (27) Hopp et al (1995), (28) Forbes, Brodie & Huchra (1997), (29) Larsen & Brodie (2000), (30) Bower et al (2001) (31) Villegas et al (2010), (32) Nowak et al (2008), (33) Hanes & Harris (1996), (34) Emsellem et al (1999), (35) Tremaine et al (2002), (36) Puzia et al (2004), (37) Gultekin et al (2009a), (38) Pignatelli, Salucci & Danese (2001), (39) Gultekin et al (2010) (40) Sarzi et al (2001), (41) Chomiuk, Strader & Brodie (2008), (42) Harris (in preparation), (43) Ghez et al (2008), (44) Gillessen et al (2009), (45) Battistini et al (1993), (46) Bender et al (2005), (47) Santiago‐Cortés, Mayya & Rosa‐González (2010), (48) Devereux et al (2003), (49) Kormendy (1988) …”

Section: The Data Basementioning

confidence: 99%

The globular cluster/central black hole connection in galaxies

Harris¹,

Harris²

2010

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We explore the relation between the total globular population in a galaxy (NGC) and the mass of its central black hole (M•). Using a sample of 33 galaxies, twice as large as the original sample discussed by Burkert & Tremaine (2010), we find that NGC for elliptical and spiral galaxies increases in almost precisely direct proportion to M•. The S0‐type galaxies by contrast do not follow a clear trend, showing large scatter in M• at a given NGC. After accounting for observational measurement uncertainty, we find that the mean relation defined by the E and S galaxies must also have an intrinsic or ‘cosmic’ scatter of ±0.2 in either log NGC or log M•. The residuals from this correlation show no trend with globular cluster specific frequency. We suggest that these two types of galaxy subsystems (central black hole and globular cluster system) may be closely correlated because they both originated at high redshift during the main epoch of hierarchical merging, and both require extremely high‐density conditions for formation. Lastly, we note that roughly 10 per cent of the galaxies in our sample (one E, one S and two S0) deviate strongly from the main trend, all in the sense that their M• is at least 10 times smaller than would be predicted by the mean relation.

show abstract

“…The powerlaw nature of SBPs at relatively younger ages is understood to be due to the contribution of stars in the unbound halo (Elson et al 1987;Moreno et al 2014). Hubble Space Telescope (HST), especially the wide field of the Advanced Camera for Surveys (ACS), has enabled the detection of large populations of SSCs in external galaxies, some examples being M82 (O'Connell et al 1995;Melo et al 2005;Mayya et al 2008), M51 (Chandar et al 2011), M81 (Chandar et al 2001;Santiago-Cortés et al 2010), M83 (Bastian et al 2011;Ryon et al 2015), and Antennae (NGC4038/4039) (Whitmore & Schweizer 1995). Clusters have been reported in 20 other nearby spiral and irregular galaxies using the Hubble Legacy Archive (HLA) data (Whitmore et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Structural analysis of disc super star clusters of M82: size and profile shape at intermediate ages

Cuevas-Otahola

Mayya

Puerari

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present the structural parameters of 99 Super Star Clusters (SSCs) in the Disk of M82. Moffat-EFF, King and Wilson models were fitted using a χ 2 minimisation method to background-subtracted Surface Brightness Profiles (SBPs) in F435W (B), F555W (V), and F814W (I) bands of the Advanced Camera for Surveys (ACS) of the Hubble Space Telescope (HST). The majority of the SSC profiles is best-fitted by the Moffat-EFF profile. The scale parameter r d and the shape parameter γ in the three filters are identical within the measurement errors. The analysed sample is big enough to allow characterisation of the distributions of core radii R c and γ. The obtained distribution of R c follows a log-normal form, with center and σlog Rc pc being 1.73 pc and 0.25, respectively. The γ distribution is also log-normal with center and σlog(γ) being 2.88 and 0.08, respectively. M82 is well-known for the absence of current star formation in its disk, with all disk SSCs older than 50 Myr and hardly any cluster older than ∼300 Myr. The derived distributions compare very well with the distributions for intermediate-age clusters in the Large Magellanic Cloud (LMC), which is also a low-mass late-type galaxy similar to M82. On the other hand, the distributions of R c in both these galaxies are shifted towards larger values as compared to SSCs of similar age in the giant spiral galaxy M83. M82 and LMC also span a narrower range of γ values as compared to that in M83.

show abstract

Wide-fieldHST/ACS images of M81: the population of compact star clusters

Cited by 24 publications

References 50 publications

The K-band luminosity functions of super star clusters in luminous infrared galaxies, their slopes and the effects of blending

The K-band luminosity functions of super star clusters in luminous infrared galaxies, their slopes and the effects of blending

The globular cluster/central black hole connection in galaxies

Structural analysis of disc super star clusters of M82: size and profile shape at intermediate ages

Contact Info

Product

Resources

About