J/AJ/131/375 Photometry and velocities of Sculptor dSph giants (Westfall+, 2006)
Exploring halo substructure with giant stars.
VIII. The extended structure of the Sculptor dwarf spheroidal galaxy.
Westfall K.B., Majewski S.R., Ostheimer J.C., Frinchaboy P.M., Kunkel W.E.,
Patterson R.J., Link R.
<Astron. J., 131, 375-406 (2006)>
=2006AJ....131..375W 2006AJ....131..375W
ADC_Keywords: Galaxies, nearby ; Radial velocities ; Photometry
Keywords: galaxies: dwarf - galaxies: halos - galaxies: individual (Sculptor) -
galaxies: photometry - galaxies: structure - Local Group
Abstract:
We explore the spatial distribution of stars in the Sculptor dwarf
spheroidal (dSph) galaxy over an area of 7.82deg2, including
coverage of the central region but extending mostly south and east of
the dSph core. Two methods are used to identify stars that are most
likely associated with the dSph, and these filtered samples of stars
are used to map its spatial structure. First, following the method of
previous contributions in this series, we utilize Washington M,
T2+DDO51 photometry to identify red giant branch (RGB) star
candidates with approximately the same distance and metallicity as
the Sculptor dSph. Second, a prominent blue horizontal branch (BHB)
population provides a fairly populous and pure sample of Sculptor
stars having broadband colors unlike the bulk of the Galactic field
star population. A spectroscopically observed subset of Sculptor
candidate stars (147 total stars: ∼5% of all Sculptor candidates
and ∼10% of Sculptor giant candidates) yields a systemic heliocentric
velocity for the system of vhel=110.43±0.79km/s, in good agreement
with previous studies.
Description:
A mosaic of the Sculptor dSph was created via CCD imaging undertaken
over the course of six observing runs at the Swope 1m telescope
located at Las Campanas Observatory, between 1999 Aug and 2001 Nov.
Spectra for this study were obtained using the HYDRA multifiber system
at the Blanco 4m telescope at the Cerro Tololo Inter-American
Observatory (CTIO) during UT 2000 November 10-12 and 2001 October
7-10. Spectra were also obtained with the Magellan Inamori Kyocera
Echelle (MIKE) slit spectrograph mounted on the Magellan II (Clay)
6.5m telescope at Las Campanas Observatory on the nights of UT 2004
January 27-28 and December 30-31.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 121 36 Adopted radial velocities for multiple observations
table4.dat 112 179 Heliocentric radial velocities of selected stars
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See also:
J/ApJ/705/328 : Abundance measurements in Sculptor dSph (Kirby+, 2009)
J/AJ/130/1065 : Members of the Sculptor dSph galaxy (Coleman+, 2005)
J/MNRAS/363/734 : Sculptor dSph variables metal abundances (Clementini+, 2005)
J/AJ/128/245 : M giant stars in the Sagittarius dwarf galaxy (Majewski+,
2004)
J/AJ/110/2747 : Stars in Sculptor dwarf spheroidal galaxy (Schweitzer+ 1995)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- ID Source identification
10- 15 F6.2 km/s HRV Average heliocentric velocity
17- 21 F5.2 km/s e_HRV Standard deviation in HRV
23- 28 F6.2 km/s HRV1 Heliocentric velocity of 1st observation
30- 33 F4.2 --- CCP1 Magnitude of the 1st observation XC peak (G1)
35 I1 --- q_Obs1 Quality (Q) of 1st observation (G1)
37- 46 A10 "YYYY/MM/DD" Obs1 UT date of 1st observation
48- 53 F6.2 km/s HRV2 Heliocentric velocity of 2nd observation
55- 58 F4.2 --- CCP2 Magnitude of the 2nd observation XC peak (G1)
60 I1 --- q_Obs2 Quality (Q) of 2nd observation (G1)
62- 71 A10 "YYYY/MM/DD" Obs2 UT date of 2nd observation
73- 78 F6.2 km/s HRV3 ? Heliocentric velocity of 3rd observation
80- 83 F4.2 --- CCP3 ? Magnitude of the 3rd observation XC peak (G1)
85 I1 --- q_Obs3 ? Quality (Q) of 3rd observation (G1)
87- 96 A10 "YYYY/MM/DD" Obs3 ? UT date of 3rd observation
98-103 F6.2 km/s HRV4 ? Heliocentric velocity of 4th observation
105-108 F4.2 --- CCP4 ? Magnitude of the 4th observation XC peak (G1)
110 I1 --- q_Obs4 ? Quality (Q) of 4th observation (G1)
112-121 A10 "YYYY/MM/DD" Obs4 ? UT date of 4th observation
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- ID Source identification
10- 11 I2 h RAh Hour of Right Ascension (J2000)
13- 14 I2 min RAm Minute of Right Ascension (J2000)
16- 20 F5.2 s RAs Second of Right Ascension (J2000)
22 A1 --- DE- Sign of the Declination (J2000)
23- 24 I2 deg DEd Degree of Declination (J2000)
26- 27 I2 arcmin DEm Arcminute of Declination (J2000)
29- 32 F4.1 arcsec DEs Arcsecond of Declination (J2000)
34- 43 A10 "YYYY/MM/DD" Obs ? UT date of observation (1)
45- 49 F5.2 mag Mmag Washington M filter magnitude
51- 54 F4.2 mag e_Mmag Uncertainty in Mmag
56- 59 F4.2 mag M-T2 Washington (M-T2) color index
61- 64 F4.2 mag e_M-T2 Uncertainty in M-T2
66- 70 F5.2 mag M-D51 Washington (M-DD051) color index
72- 75 F4.2 mag e_M-D51 Uncertainty in M-D51
77- 83 F7.2 km/s HRV Heliocentric velocity
85- 88 F4.2 km/s e_HRV ? The 1σ error in HRV (2)
90- 93 F4.2 --- CCP ? Magnitude of the XC peak (G1)
95 I1 --- q_Obs ? Quality (Q) (G1)
97-104 F8.4 arcmin Dist Elliptical distance (3)
106 A1 --- P [Y/N] Satisfies the photometric criterion
108 A1 --- f_P Remarks on the photometric selection (4)
110 A1 --- V [Y/N] Satisfies the radial velocity criterion
112 A1 --- f_V [j] Remarks on the velocity selection (4)
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Note (1): Dates for stars multiply observed by us are given in Table 2.
Note (2): Errors from literature stars, calculated for multiply observed
stars as: (∑[1/ε(vi)2])-1/2.
Errors for stars observed by us on Nov 2000, Oct 2001, Jan 2004, and
Dec 2004 are adopted as 10, 4, 1.5, and 2.5km/s, respectively.
Note (3): Assuming the mean ellipticity for the samples fit in Section 5.2.
Note (4): Flag as follows:
e = Star selected as giant candidate but fell redward of our RGB/RHB
selection at the bright end.
f = Previously observed star that is consistent with our photometric
candidate constraints but does not satisfy our χ morphological
constraint.
g = Photometrically selected BHB candidate.
h = Star fell redward of our BHB selection.
i = Star fell blueward of our 2CD selection limit.
j = Mean HRV inconsistent with Sculptor but at least one individual
observation was consistent.
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Global notes:
Note (G1): Velocities are determined via a modified version of the
cross-correlation (XC) technique developed initially by Tonry & Davis
(1979AJ.....84.1511T 1979AJ.....84.1511T); the methology is described by Majewski et al.
2004 (Paper VI, see Cat. J/AJ/128/245). The qualities are gauged by
the strength (as compared to secondary peaks) and symmetry of the XC
peak on a scale Q=1 (lowest) to Q=7 (highest) quality.
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History:
From electronic version of the journal
References:
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Majewski et al. Paper II. 2000AJ....119..760M 2000AJ....119..760M
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(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 27-Jun-2011