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 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:
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FileName Lrecl Records Explanations
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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
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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
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Bytes Format Units Label Explanations
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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
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Note (1): Represents the weighted average of the individually measured
velocity values that follow.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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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)
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Note (1): Observational flag, defined as follows:
b = Multiple Exposures, see Table 3.
e = Stars from Mateo et al. (1993AJ....105..510M 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.
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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.
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History:
From electronic version of the journal
References:
Majewski et al., Paper I 2000AJ....120.2550M 2000AJ....120.2550M
Majewski et al., Paper II 2000AJ....119..760M 2000AJ....119..760M
Kundu et al., Paper III 2002ApJ...576L.125K 2002ApJ...576L.125K
Palma et al., Paper IV 2003AJ....125.1352P 2003AJ....125.1352P, Cat. J/AJ/125/1352
Crane et al. 2003ApJ...594L.119C 2003ApJ...594L.119C
Rocha-Pinto et al. 2004ApJ...615..732R 2004ApJ...615..732R
Munoz et al. 2005ApJ...631L.137M 2005ApJ...631L.137M
Westfall et al., Paper VIII 2006AJ....131..375W 2006AJ....131..375W
Munoz et al. 2006ApJ...650L..51M 2006ApJ...650L..51M
Sohn et al., Paper X 2007ApJ...663..960S 2007ApJ...663..960S, Cat. <J/ApJ/663/960 >
Munoz et al., Paper XI 2006ApJ...649..201M 2006ApJ...649..201M, Cat. J/ApJ/649/201
Majewski et al. 2012ApJ...747L..37M 2012ApJ...747L..37M
Sheffield et al., Paper XIV 2014ApJ...793...62S 2014ApJ...793...62S, Cat. J/ApJ/793/62
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 07-Aug-2006