J/AJ/130/2677 Stars in the Carina dSph galaxy field (Majewski+, 2005)
Exploring halo substructure with giant stars. VI. Extended distributions of giant stars around the Carina dwarf spheroidal galaxy: how reliable are they? Majewski S.R., Frinchaboy P.M., Kunkel W.E., Link R., Munoz R.R., Ostheimer J.C., Palma C., Patterson R.J., Geisler D. <Astron. J., 130, 2677-2700 (2005)> =2005AJ....130.2677M
ADC_Keywords: Radial velocities ; Galaxies, spectra ; Photometry, CMT1T2V ; Stars, giant Keywords: galaxies: individual (Carina) - Galaxy: evolution - Galaxy: halo - Galaxy: structure - methods: statistical - techniques: photometric Abstract: The question of the existence of active and prominent tidal disruption around various Galactic dwarf spheroidal (dSph) galaxies remains controversial. That debate often centers on the nature (bound vs. unbound) of extended populations of stars claimed to lie outside the bounds of single King profiles fitted to the density distributions of dSph centers. However, the more fundamental issue of the very existence of the previously reported extended populations is still contentious. We present a critical evaluation of the debate centering on one particular dSph, Carina, for which claims both for and against the existence of stars beyond the King limiting radius have been made. Description: Spectra of our Carina giant candidates have been obtained using the Blanco 4m + Hydra multifiber spectrograph system at the Cerro Tololo Inter-American Observatory on the nights of UT 2000 March 26-29, 2000 November 10-12, and 2001 October 8-11. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 39 72 Stars in Carina field with repeat Hydra observations table5.dat 83 133 Radial velocities of stars in the Carina field
See also: J/AJ/125/1352 : Ursa Minor dSph M,T2, DDO51 photometry (Palma+, 2003) J/AJ/114/1458 : The Carina Dwarf (Mighell 1997) J/ApJ/663/960 : Radial velocities of Leo I stars (Sohn+, 2007) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 8 A8 --- [MOP2000] Star Name ([MOP2000] CNNNNNNN in Simbad) 10- 14 F5.1 km/s RV Radial velocity 16 A1 --- n_RV [a] Indicates a final adopted RV (1) 18- 21 F4.2 --- CCP ? Height of the cross-correlation peak 23 I1 --- Q Quality factor (G1) 25- 28 F4.1 km/s e_RV ? Standard deviation on RV 30- 39 A10 "DD/MM/YYYY" ObsDate ? Date of the observation
Note (1): Represents the weighted average of the individually measured velocity values that follow.
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 8 A8 --- [MOP2000] Star name 10 I1 h RAh Hour of Right Ascension (J2000) 12- 13 I2 min RAm Minute of Right Ascension (J2000) 15- 19 F5.2 s RAs Second of Right Ascension (J2000) 21 A1 --- DE- Sign on the Declination (J2000) 22- 23 I2 deg DEd Degree of Declination (J2000) 25- 26 I2 arcmin DEm Arcminute of Declination (J2000) 28- 31 F4.1 arcsec DEs Arcsecond of Declination (J2000) 33- 42 A10 "DD/MM/YYYY" ObsDate ? Date of the observation 44 A1 --- n_ObsDate [be] Observational flag (1) 46- 50 F5.2 mag Mmag Washington dereddened M0 band magnitude 52- 56 F5.2 mag M-T2 Washington dereddened (M-T2)0 color index 58- 62 F5.2 mag M-51 Dereddened (M-DD051)0 color index 64- 69 F6.1 km/s HRV Heliocentric radial velocity 71- 74 F4.2 --- CCP ? Height of the cross-correlation peak 76 A1 --- Q Quality factor (G1) 78 A1 --- Cand [YN] Originally selected to be a Carina giant? (2) 80- 81 A2 --- Memb [YN? ] Final judgement as a true Carina system member? (2) 83 A1 --- f_Memb [acd] Membership notes (3)
Note (1): Observational flag, defined as follows: b = Multiple Exposures, see Table 3. e = Stars from Mateo et al. (1993AJ....105..510M) not observed by us. Note (2): Flag defined as follows: Y = Yes; N = No; ? = Unknown. Note (3): Flag on Memb, defined as follows: a = Possible PAGB Carina star (see Section 3.3.3.). c = Star was just outside our RGB selection boundary, but has the correct RV and is also selected as a giant in the 2CD. d = Star has correct RV but is not considered a member because of location in the CMD.
Global Notes: Note (G1): Depending on the strength and shape of the correlation peak with respect to other features in the cross-correlation function, with Q=7 being a solid RV measurement and Q=4 the lowest quality cross-correlation that yields a trustworthy RV.
History: From electronic version of the journal References: Majewski et al., Paper I 2000AJ....120.2550M Majewski et al., Paper II 2000AJ....119..760M Kundu et al., Paper III 2002ApJ...576L.125K Palma et al., Paper IV 2003AJ....125.1352P, Cat. J/AJ/125/1352 Crane et al. 2003ApJ...594L.119C Rocha-Pinto et al. 2004ApJ...615..732R Munoz et al. 2005ApJ...631L.137M Westfall et al., Paper VIII 2006AJ....131..375W Munoz et al. 2006ApJ...650L..51M Munoz et al., Paper XI 2006ApJ...649..201M, Cat. J/ApJ/649/201 Sohn et al., Paper X 2007ApJ...663..960S, Cat. <J/ApJ/663/960 >
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 07-Aug-2006
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