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J/MNRAS/448/1314    Line list for seven target PAndAS clusters   (Sakari+, 2015)

Integrated light chemical tagging analyses of seven M31 outer halo globular clusters from the Pan-Andromeda Archaeological Survey. Sakari C.M., Venn K.A., Mackey D., Shetrone M.D., Dotter A., Ferguson A.M.N., Huxor A. <Mon. Not. R. Astron. Soc., 448, 1314-1334 (2015)> =2015MNRAS.448.1314S (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Clusters, globular ; Magnitudes ; Abundances, [Fe/H] ; Spectroscopy ; Equivalent widths Keywords: globular clusters: general - galaxies: abundances - galaxies: evolution - galaxies: individual: M31 - galaxies: star clusters: general Abstract: Detailed chemical abundances are presented for seven M31 outer halo globular clusters (with projected distances from M31 greater than 30 kpc), as derived from high-resolution integrated light spectra taken with the Hobby-Eberly Telescope. Five of these clusters were recently discovered in the Pan-Andromeda Archaeological Survey (PAndAS) - this paper presents the first determinations of integrated Fe, Na, Mg, Ca, Ti, Ni, Ba, and Eu abundances for these clusters. Four of the target clusters (PA06, PA53, PA54, and PA56) are metal poor ([Fe/H]< -1.5), α-enhanced (though they are possibly less α-enhanced than Milky Way stars at the 1σ level), and show signs of star-to-star Na and Mg variations. The other three globular clusters (H10, H23, and PA17) are more metal rich, with metallicities ranging from [Fe/H]=-1.4 to -0.9. While H23 is chemically similar to Milky Way field stars, Milky Way globular clusters, and other M31 clusters, H10 and PA17, have moderately low [Ca/Fe], compared to Milky Way field stars and clusters. Additionally, PA17's high [Mg/Ca] and [Ba/Eu] ratios are distinct from Milky Way stars, and are in better agreement with the stars and clusters in the Large Magellanic Cloud. None of the clusters studied here can be conclusively linked to any of the identified streams from PAndAS; however, based on their locations, kinematics, metallicities, and detailed abundances, the most metal-rich PAndAS clusters H23 and PA17 may be associated with the progenitor of the Giant Stellar Stream, H10 may be associated with the SW cloud, and PA53 and PA56 may be associated with the eastern cloud. Description: The targets were observed with the Hobby-Eberly Telescope (HET; Ramsey et al. 1998, Proc. SPIE, 3352, 34; Shetrone et al. 2007PASP..119..556S) at McDonald Observatory in Fort Davis, TX in 2011 and early 2012. The High Resolution Spectrograph (HRS; Tull 1998, Proc. SPIE, 3355, 387) was utilized with the 3-arcsec fibre and a slit width of 1 arcsec, yielding an instrumental spectral resolution of R=30000. With the 600 g/mm cross-disperser set to a central wavelength of 6302.9Å, wavelength coverages of ∼5320-6290 and ∼6360-7340Å were achieved in the blue and the red, respectively. The 3-arcsec fibre provided coverage of the clusters past their half-light radii; the additional sky fibres (located 10 arcsec from the central object fibre) provided simultaneous observations for sky subtraction. Exposure times were calculated to obtain a total signal-to-noise ratio (S/N)=80 (per resolution element), although not all targets received sufficient time to meet this goal. Objects: ---------------------------------------------------- RA (ICRS) DE Designation(s) ---------------------------------------------------- 00 42 44.33 +41 16 07.5 M31 = NAME Andromeda ---------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 61 7 Properties of the target PAndAS clusters table3.dat 68 129 The Line List
See also: V/143 : Revised Bologna Catalog of M31 clusters, V.5 (Galleti+ 2012) J/AJ/122/2458 : M31 globular clusters from HST (Barmby+, 2001) J/AJ/124/234 : M31 outer halo UBVRI photometry and metallicity (Reitzel+, 2002) J/AJ/133/2764 : M31 globular clusters structural parameters (Barmby+, 2007) J/A+A/508/1285 : Metallicity estimates of M31 globular clusters (Galleti+, 2009) J/A+A/544/A155 : HST photometry of M31 globular clusters (Federici+, 2012) J/A+A/549/A60 : Ages and [Fe/H] of M31 globular clusters (Cezario+, 2013) J/ApJ/769/10 : Spectroscopy of M31 globular clusters (Jacoby+, 2013) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 4 A4 --- Name PAndAS cluster name 6- 7 I2 h RAh Hour of Right Ascension (J2000) 9- 10 I2 min RAm Minute of Right Ascension (J2000) 12- 15 F4.1 s RAs Second of Right Ascension (J2000) 17 A1 --- DE- Sign of the Declination (J2000) 18- 19 I2 deg DEd Degree of Declination (J2000) 21- 22 I2 arcmin DEm Arcminute of Declination (J2000) 24- 27 F4.1 arcsec DEs Arcsecond of Declination (J2000) 29- 32 F4.1 mag Vint Integrated V-band magnitude 34- 38 F5.1 kpc Rproj Projected distance from the centre of M31 40- 44 A5 [-] [Fe/H] Photometric metallicity estimate (1) 45 A1 --- n_[Fe/H] [c] Note on [Fe/H] (2) 47- 55 A9 --- Assoc Spatial association with stream? (N=No) 57- 61 A5 --- Ref Reference(s) (3)
Note (1): Used to constrain the parameters of the input isochrones; see Section 3. [Fe/H] estimates are based on Galactic GC fiducial fits. "MP" indicates a metal-poor cluster ([Fe/H]~< -1.5); fiducial fits will be given in Mackey et al. (2016MNRAS.460L.114M). Note (2): Note as follows: c = PA17 does not have an HST CMD, and there is therefore no a priori information about its metallicity or horizontal branch (HB) morphology. Note (3): Reference as follows: 1 = Mackey et al. (2007ApJ...655L..85M); 2 = Veljanoski et al. (2014MNRAS.442.2929V); 3 = Huxor et al. (2014MNRAS.442.2165H); 4 = Mackey et al. (2016MNRAS.460L.114M).
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 8 F8.3 0.1nm lambda Spectral line wavelength (Å) 10- 13 A4 --- El Element and ionization state 15- 19 F5.3 eV EP Excitation Potential 21- 26 F6.3 [-] loggf Oscillator strength 28- 32 F5.1 0.1pm EW-H10 ?=- H10 equivalent width (mÅ) 33 A1 --- n_EW-H10 [s] Mote on EW-H10 (1) 34- 38 F5.1 0.1pm EW-H23 ?=- H23 equivalent width (mÅ) 39 A1 --- n_EW-H23 [s] Mote on EW-H23 (1) 40- 44 F5.1 0.1pm EW-PA06 ?=- PA06 equivalent width (mÅ) 45 A1 --- n_EW-PA06 [s] Mote on EW-PA06 (1) 46- 50 F5.1 0.1pm EW-PA17 ?=- PA17 equivalent width (mÅ) 51 A1 --- n_EW-PA17 [s] Mote on EW-PA17 (1) 52- 56 F5.1 0.1pm EW-PA53 ?=- PA53 equivalent width (mÅ) 57 A1 --- n_EW-PA53 [s] Mote on EW-PA53 (1) 58- 61 F4.1 0.1pm EW-PA54 ?=- PA54 equivalent width (mÅ) 62 A1 --- n_EW-PA54 [s] Mote on EW-PA54 (1) 63- 67 F5.1 0.1pm EW-PA56 ?=- PA56 equivalent width (mÅ) 68 A1 --- n_EW-PA56 [s] Mote on EW-PA56 (1)
Note (1): s indicates that the lines were measured with spectrum syntheses.
History: From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 21-Nov-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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