The Main-Sequence Stars of the Sagittarius Dwarf Galaxy

Fahlman, Gregory G.; Mandushev, Georgi; Richer, Harvey B.; Thompson, I. B.; Sivaramakrishnan, A.

doi:10.1086/309955

Cited by 47 publications

(51 citation statements)

References 21 publications

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“…The Sgr dwarf tails have been shown to have a main sequence turn off of V MSTO ∼ 21 (e.g. Fahlman et al 1996;Majewski et al 1999). Since, in our CMD, these objects are relatively blue, we expect (V − R) > 0 and, therefore, if this sequence was the MSTO of stars in the Sgr dwarf tidal tail we find that V MSTO > 22.…”

Section: Point Source Colour-magnitude Diagramsmentioning

confidence: 49%

Isolated ellipticals and their globular cluster systems

Salinas¹,

Richtler²

2013

A&A

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The globular cluster (GC) systems of isolated elliptical galaxies have only recently begun to be studied in detail, and may exhibit morphological connections to the evolutionary histories of their hosts. Here we present the first in a series of wide-field analyses of the GC systems of the isolated ellipticals -Washington C and R photometry of NGC 3585 and NGC 5812 down to R ∼ 24 mag. The GC systems are characterised, with each system displaying both the "Universal" blue peak at (C − R) ∼ 1.3, and a red peak, but each with differing strengths. The total number of GCs in each system, and their specific frequencies, are estimated. The GC colours and specific frequencies are highly indicative that the host galaxy environment plays a role in shaping its GC system. We produce, and subtract, accurate models of each galaxy, revealing interesting underlying features, including the first definitive evidence that NGC 5812 is interacting with a dwarf companion galaxy. From the galaxy models we also determine surface brightness and colour profiles. Both colour profiles appear quite flat and with (C − R) ∼ 1.7 and we discuss the apparent youth of NGC 3585 in the context of this work.

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Section: Point Source Colour-magnitude Diagramsmentioning

confidence: 49%

Isolated ellipticals and their globular cluster systems

Salinas¹,

Richtler²

2013

A&A

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“…Three of the observed SX Phe type stars: V28, V29, V30, are 3.5-4 mag fainter than the rest of our sample stars. This difference in magnitude places these 3 stars in the Sagittarius dwarf galaxy (Ibata et al 1994;Fahlman et al 1996). The 24 remaining SX Phe variables constitute approximately 50 percent of all the blue straggler stars present in our data.…”

Section: Identification Of Variablesmentioning

confidence: 72%

Cluster AgeS Experiment. CCD photometry of SX Phoenicis variables in the globular cluster M 55

Pych

Kałużny

Krzemiński

et al. 2001

A&A

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Abstract. We present CCD photometry of SX Phe variables in the field of the globular cluster M 55. We have discovered 27 variables, three of which are probable members of the Sagittarius dwarf galaxy. All of the SX Phe stars in M 55 lie in the blue straggler region of the cluster color-magnitude diagram. Using period ratio information we have identified the radial pulsation modes for one of the observed variables. Inspection of the period-luminosity distribution permits the probable identifications of the pulsation modes for most of the rest of the stars in the sample. We have determined the slope of the period-luminosity relation for SX Phe stars in M 55 pulsating in the fundamental mode. Using this relation and the HIPPARCOS data for SX Phe itself, we have estimated the apparent distance modulus to M 55 to be (m − M )V = 13.86 ± 0.25 mag.

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“…However, the number of these stars and their distribution in azimuth and radius remain uncertain because of the incomplete areal coverage and variable limiting magnitudes of the M2K Ðelds, and the concerns raised by Morrison et al Since the discovery of the Sagittarius dSph (Ibata, Gilmore, & Irwin 1994), stars associated with this galaxy have been found at ever-increasing angular distances from its center. Mateo et al (1996) and Fahlman et al (1996) found main-sequence stars of Sagittarius about 10¡ from the center. Mateo et al (1996) also found RR Lyrae stars associated with Sagittarius in their Ðeld, as did Alard (1996) and Alcock et al (1997) in Ðelds 8¡ to 11¡ from the center on the opposite side.…”

Section: Summary and Discussionmentioning

confidence: 99%

Stars of the Draco Dwarf Spheroidal Galaxy Beyond Its Measured Tidal Boundary

Piatek

Pryor

Armandroff³

et al. 2001

The Astronomical Journal

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We report R-and V -band photometry derived from CCD imaging for objects in nine Ðelds in and around the Draco dwarf spheroidal galaxy. The most distant Ðelds are about from the center. We 1¡ .3 use these data to search for Draco stars outside of its measured tidal boundary. The search involves three methods : (1) plotting color-magnitude diagrams for individual Ðelds, for sections of Ðelds, and for combined Ðelds and sectionsÈa colour-magnitude diagram can reveal a population of Draco stars by the presence of the expected principal sequences ; (2) measuring Ðeld-to-Ðeld Ñuctuations in the surface density of objects located near the Draco principal sequences in the color-magnitude diagram ; (3) measuring intraÐeld Ñuctuations in the surface density of those objects. We Ðnd evidence for the presence of Draco stars immediately beyond the measured tidal boundary of Draco and place an upper limit on the number of such stars in more distant Ðelds that lie close to the extension of its major axis. The best evidence is the presence of the Draco principal sequences in the color-magnitude diagram for some combined Ðelds and sections of Ðelds. The measurements of the Ðeld-to-Ðeld Ñuctuations in the stellar surface density conÐrm this result.

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The Main-Sequence Stars of the Sagittarius Dwarf Galaxy

Cited by 47 publications

References 21 publications

Isolated ellipticals and their globular cluster systems

Isolated ellipticals and their globular cluster systems

Cluster AgeS Experiment. CCD photometry of SX Phoenicis variables in the globular cluster M 55

Stars of the Draco Dwarf Spheroidal Galaxy Beyond Its Measured Tidal Boundary

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