The Structure of the Fornax Dwarf Galaxy

Hodge, P. W.; Smith, D. W.

doi:10.1086/152678

Cited by 14 publications

(17 citation statements)

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“…Our estimate of the position of the peak density in Fornax, as given by the centroid of the 500 pixel circle, lies some 0Ј .5 west and 2Ј .5 north of cluster 4 (whose position is 02 h 40 m 10 s , Ϫ34Њ31Ј34Љ [2000.0] according to Hodge & Smith). This is similar to the estimates of Hodge (1961b) and Hodge & Smith (1974), but distinct from the claim of Demers & Irwin, who said that the peak of Fornax coincides with cluster 4.…”

Section: Overall Spatial Distributionsupporting

confidence: 88%

Homogeneous Photometry for Star Clusters and Resolved Galaxies. I. A Survey of Bright Stars in the Fornax Dwarf Spheroidal Galaxy

Stetson

Hesser

Smecker-Hane

1998

PUBL ASTRON SOC PAC

152

240

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ABSTRACT. We present accurate photometry on the Johnson B, Kron-Cousins R photometric system for approximately 100,000 stars in a deg 2 field centered on the dwarf spheroidal galaxy in Fornax. We identify 1 3 numerous probable short-period variable stars, blue stars that appear to be the main sequence of a small population with an age of order 10 8 yr, and two distinct types of luminous red star: an extended sequence of primarily carbon stars and a clump of mostly M giants slightly more luminous than the giant-branch tip. The spatial distribution of each of these subpopulations within the Fornax dwarf galaxy is considered.

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Section: Overall Spatial Distributionsupporting

confidence: 88%

Homogeneous Photometry for Star Clusters and Resolved Galaxies. I. A Survey of Bright Stars in the Fornax Dwarf Spheroidal Galaxy

Stetson

Hesser

Smecker-Hane

1998

PUBL ASTRON SOC PAC

152

240

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“…Hodge constructed a radial profile and contour plot for Fornax, noting two main points concerning its structure: (1) ellipticity increased with increasing radius, and (2) it was characterized by an asymmetry such that the point of highest density was offset from the center by $6 0 . Two later studies (de Vaucouleurs & Ables 1968;Hodge & Smith 1974) used photoelectric surface photometry to map the structure of Fornax. Both confirmed the asymmetry found by Hodge (1961b); however, these studies were hindered by the faint surface brightness of Fornax.…”

Section: Structurementioning

confidence: 99%

A Wide-Field Survey of the Fornax Dwarf Spheroidal Galaxy

Coleman¹,

Costa²,

Bland-Hawthorn³

et al. 2005

127

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The results of a photometric survey of the Fornax dwarf spheroidal galaxy are presented herein. Accurate photometry in two colours (V and I) was collected over a 10 square degree area centred on the Fornax system with the aim of searching for extra-tidal structure. The data were complete to a magnitude of V=20, or approximately one magnitude brighter than the Fornax red clump stars. Stars were selected with a colour and magnitude lying near the Fornax red giant branch, thereby reducing contamination from the field star population. We were thus able to probe the outer structure of this dwarf galaxy. Immediately visible was a shell-like structure located 1.3 degrees NW from the centre of Fornax, approximately 30 arcmin beyond the nominal tidal radius at this position angle. We have measured the absolute visual magnitude of this feature to be M_V ~ -7. The feature is aligned with a previously reported shell (age approximately 2 Gyr) located near the core radius of Fornax. A statistical analysis of the extra-tidal stellar distribution further revealed two lobes situated on the Fornax minor axis which are aligned with the two shell-like features. The two-lobed structure combined with the two shells provide strong evidence that Fornax has experienced a merger event in the relatively recent past.Comment: 79 pages including 24 figures. Accepted for publication in AJ, scheduled for the March 2005 issue. Some figures are low resolution, and a full version of the paper is available at the ftp address: ftp://ftp.mso.anu.edu.au/pub/coleman

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“…Bahcall & Wolf 1976;Gurzadyan 1982;Merritt et al 2006) where r c is the core radius and M BH the black hole mass. In particular, the green diamonds (with labels SHS98 500 pxl and SHS98 2000 pxl) correspond to the galaxy centers obtained by Stetson et al (1998), the red and black diamonds indicate the centroids as derived by Hodge & Smith (1974) and Demers & Irwin (1987), respectively (see text for details).…”

Section: An Intermediate-mass Black Hole In the Fornax Galaxy: High-ementioning

confidence: 99%

“…6. In the same figure, we also give the coordinates of the centroid as obtained by Hodge & Smith (1974;red diamond) and Demers & Irwin (1987;black diamond). For comparison, the yellow diamond (on a CCD gap of the pn camera) represents the centroid as recently determined by Battaglia et al (2006) and the blue diamond is centered on the NED coordinates of Fornax dSph.…”

Section: An Intermediate-mass Black Hole In the Fornax Galaxy: High-ementioning

confidence: 99%

“…We then accumulated the background on a region located on the 17 In the case in which the Fornax centroid position coincides with one of those evaluated by Hodge & Smith (1974), Demers & Irwin (1987), or Battaglia et al (2006) (red, black, and yellow diamonds in Fig. 6, respectively), we can set only an upper limit to the IMBH unabsorbed flux of 2.5 × 10 −15 erg s −1 cm −2 which, at the distance of the Fornax dSph, corresponds to a luminosity limit of 5.7 × 10 33 erg s −1 .…”

Section: An Intermediate-mass Black Hole In the Fornax Galaxy: High-ementioning

confidence: 99%

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AnXMM-Newtonsearch for X-ray sources in the Fornax dwarf galaxy

Nucita

Manni

Paolis

et al. 2013

A&A

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We report the results of a deep archive XMM-Newton observation of the Fornax spheroidal galaxy that we analyzed with the aim of fully characterizing the X-ray source population (in most of the cases likely to be background active galactic nuclei) detected towards the target. A cross correlation with the available databases allowed us to find a source that may be associated with a variable star belonging to the galaxy. We also searched for X-ray sources in the vicinity of the Fornax globular clusters GC 3 and GC 4 and found two sources probably associated with the respective clusters. The deep X-ray observation was also suitable for the search of the intermediate-mass black hole (of mass 10 4 M ) expected to be hosted in the center of the galaxy. In the case of Fornax, this search is extremely difficult since the galaxy centroid of gravity is poorly constrained because of the large asymmetry observed in the optical surface brightness. Since we cannot firmly establish the existence of an X-ray counterpart of the putative black hole, we put constraints only on the accretion parameters. In particular, we found that the corresponding upper limit on the accretion efficiency, with respect to the Eddington luminosity, is as low as a few 10 −5 .

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The Structure of the Fornax Dwarf Galaxy

Cited by 14 publications

References 0 publications

Homogeneous Photometry for Star Clusters and Resolved Galaxies. I. A Survey of Bright Stars in the Fornax Dwarf Spheroidal Galaxy

Homogeneous Photometry for Star Clusters and Resolved Galaxies. I. A Survey of Bright Stars in the Fornax Dwarf Spheroidal Galaxy

A Wide-Field Survey of the Fornax Dwarf Spheroidal Galaxy

AnXMM-Newtonsearch for X-ray sources in the Fornax dwarf galaxy

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