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Detailed Description of J/AJ/149/7 :
SDSS-III/APOGEE. I. Be stars (Chojnowski+, 2015)

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Note : this is the description file of the original catalog. This HTML page corresponds well to the original description, but some minor changes in the format may have been introduced in the FITS output files in order to allow for arithmetic operations on quantities such as coordinates and times. h:m:s and d:m:s units are normally converted into degrees, and YYYY-MM-DD into julian days.
Similarly, some slight changes may have been introduced in the units; the value given in the HTML files supersedes the value indicated in the ReadMe file for this catalogue.
J/AJ/149/7            SDSS-III/APOGEE. I. Be stars           (Chojnowski+, 2015)
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High-resolution H-band spectroscopy of Be stars with SDSS-III/APOGEE:
I. New Be stars, line identifications, and line profiles.
    Chojnowski S.D., Whelan D.G., Wisniewski J.P., Majewski S.R., Hall M.,
    Shetrone M., Beaton R., Burton A., Damke G., Eikenberry S., Hasselquist S.,
    Holtzman J.A., Meszaros S., Nidever D., Schneider D.P., Wilson J.,
    Zasowski G., Bizyaev D., Brewington H., Brinkmann J., Ebelke G.,
    Frinchaboy P.M., Kinemuchi K., Malanushenko E., Malanushenko V.,
    Marchante M., Oravetz D., Pan K., Simmons A.
   <Astron. J., 149, 7 (2015)>
   =2015AJ....149....7C
================================================================================
ADC_Keywords: Stars, Be ; Stars, emission ; Spectroscopy ; Spectral types

Keywords: circumstellar matter - infrared: stars - line: identification -
          line: profiles - stars: early-type - stars: emission-line, Be

Abstract:
    The Apache Point Observatory Galactic Evolution Experiment (APOGEE)
    has amassed the largest ever collection of multi-epoch,
    high-resolution (R~22500), H-band spectra for B-type emission line
    (Be) stars. These stars were targeted by APOGEE as telluric standard
    stars and subsequently identified via visual inspection as Be stars
    based on HI Brackett series emission or shell absorption in addition
    to otherwise smooth continua and occasionally non-hydrogen emission
    features. The 128/238 APOGEE Be stars for which emission had never
    previously been reported serve to increase the total number of known
    Be stars by ~6%. Because the H band is relatively unexplored compared
    to other wavelength regimes, we focus here on identification of the
    H-band lines and analysis of the emission peak velocity separations
    ({Delta}vp) and emission peak intensity ratios (V/R) of the
    usually double-peaked HI and non-hydrogen emission lines. HI Br11
    emission is found to preferentially form in the circumstellar disks at
    an average distance of ~2.2 stellar radii. Increasing {Delta}vp
    toward the weaker Br12-Br20 lines suggests these lines are formed
    interior to Br11. By contrast, the observed IR FeII emission lines
    present evidence of having significantly larger formation radii;
    distinctive phase lags between IR FeII and HI Brackett emission lines
    further supports that these species arise from different radii in Be
    disks. Several emission lines have been identified for the first time
    including CI 16895, a prominent feature in the spectra for almost a
    fifth of the sample and, as inferred from relatively large
    {Delta}vp compared to the Br11-Br20, a tracer of the inner
    regions of Be disks. Emission lines at 15760Å and 16781Å remain
    unidentified, but usually appear along with and always have similar
    line profile morphology to FeII 16878. Unlike the typical metallic
    lines observed for Be stars in the optical, the H-band metallic lines,
    such as FeII 16878, never exhibit any evidence of shell absorption,
    even when the HI lines are clearly shell-dominated. The first known
    example of a quasi-triple-peaked Br11 line profile is reported for
    HD253659, one of several stars exhibiting intra- and/or extra-species
    V/R and radial velocity variation within individual spectra. Br11
    profiles are presented for all discussed stars, as are full APOGEE
    spectra for a portion of the sample.

Description:
    The sample at hand consists of 238 B-type emission line (Be) stars
    that have been observed by APOGEE.

    The Apache Point Observatory Galactic Evolution Experiment (APOGEE)
    instrument is a 300 fiber, R~22500 spectrograph attached to the SDSS
    2.5m telescope at Apache Point Observatory. APOGEE records a vacuum
    wavelength range of 15145-16955Å via an arrangement of three
    Teledyne H2RG 2048*2048 detectors. The detector layout consists of
    "blue," "green," and "red" detectors which cover 15145-15808Å,
    15858-16433Å, and 16474-16955Å respectively, resulting in
    coverage gaps between 15808-15858Å and 16433-16474Å.

    The APOGEE survey uses the Two Micron All Sky Survey (2MASS; cat. II/246)
    as a source catalog.

    Both proprietary and publicly available spectra are used and displayed
    in this paper. The publicly available spectra were included in SDSS
    data release 10 (DR10: pertains to APOGEE data taken prior to
    MJD=56112), and the full data set will be made publicly available in
    SDSS data release 12 (DR12: scheduled for 2014 December). Shortly
    after DR12, we intend to convert the ABE star spectra to the format
    accepted by the Be Star Spectra Database (BeSS; Neiner et al.,
    2011AJ....142..149N) and deposit them there, ensuring convenient
    public access. More details on DR10-released APOGEE data can be found
    on the SDSS-III website (http://www.sdss3.org/dr10/irspec/).

File Summary:

FileName Lrecl Records Explanations
× 80 . This file × ReadMe 80 . This file × tablea1.dat 130 261 List of ABE (APOGEE Be) stars × refs.dat 70 77 References
See also: B/mk : Catalogue of Stellar Spectral Classifications (Skiff, 2009-2014) http://www.sdss3.org/dr10/irspec/ : SDSS-III website J/AJ/148/24 : Extinction maps in the bulge from APOGEE (Schultheis+, 2014) J/AJ/146/156 : APOGEE M-dwarf survey. I. 1st yr velocities (Deshpande+, 2013) J/AJ/146/133 : Stellar parameters from SDSS-III APOGEE DR10 (Meszaros+, 2013) J/other/BASI/39.517 : Spectroscopy of classical Be stars (Mathew+, 2011) J/ApJ/700/1216 : Spectroscopy of Be stars in open clusters (McSwain+, 2009) J/A+A/459/137 : Bright Be shell stars (Rivnius+, 2006) J/A+A/451/1053 : Fundamental parameters of Be stars (Fremat+, 2006) J/A+A/378/861 : Spectroscopy of Be stars (Chauville+, 2001) Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1 A1 --- n_ABE [TAQ] Group of ABE stars (1) 3- 5 A3 --- ABE Identifier of the APOGEE B-type emission line (Be) star (2) 7- 9 A3 --- New Indicates a newly identified Be star 11- 26 A16 --- 2MASS 2MASS identifier (Cat. II/246) 28- 33 I6 --- HD ? HD identifier 35- 50 A16 --- Name Common star name 52- 56 F5.2 mag Vmag V band magnitude from SIMBAD database 58- 63 F6.3 mag Hmag 2MASS H band magnitude 65- 75 A11 --- SpT Literature spectral type 77- 80 A4 --- f_SpT Indicates that the original source of the spectral type could not be tracked down (3) 82- 83 I2 --- r_SpT ? Reference on SpT where available; in refs.dat file 85 A1 --- l_dVBr11 [<] Upper limit flag on dVBr11 86- 89 I4 km/s dVBr11 ? Mean velocity separation of the violet and red emission peaks {Delta}vp of Br11 1.6811µm 91- 96 A6 --- f_dVBr11 No velocity despite line detection (4) 98-100 I3 km/s dV15760 ? {Delta}vp of 1.5760µm emission 102-103 A2 --- f_dV15760 No velocity despite line detection (4) 105-107 I3 km/s dV16781 ? {Delta}vp of 1.6781µm emission 109-110 A2 --- f_dV16781 No velocity despite line detection (4) 112-113 I2 km/s dV16792 ? {Delta}vp of FeII 1.6792µm emission 115-116 A2 --- f_dV16792 No velocity despite line detection (4) 118-120 I3 km/s dV16878 ? {Delta}vp of FeII 1.6878µm emission 122-123 A2 --- f_dV16878 No velocity despite line detection (4) 125-127 I3 km/s dVCI ? {Delta}vp of CI 1.6895µm emission 129-130 A2 --- f_dVCI No velocity despite line detection (4)
Note (1): The APOGEE B-type emission line (ABE) identifiers were assigned to avoid the use of sometimes lengthy survey identifiers which are the only star names available. Three groups of ABE stars are distinguished from one another by ABE identifier as follows: T = Be stars that were quasi-randomly targeted by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) as telluric standard stars (TSS) and subsequently identified as Be stars through visual inspection of the wavelength region encompassing Br11 and FeII 16878. To account for sources only producing emission lines in certain epochs, which was frequently the case, it was necessary to examine all >70000 individual spectra for all >17000 telluric stars; A = Be stars that we targeted intentionally via internal proposals for APOGEE observations of ancillary (hence the "A" prefix of the ABE IDs) science targets falling within a subset of pre-planned APOGEE fields. Most of the intentionally targeted Be stars are early-type (B3 and hotter) classical Be stars, showing stronger than average H-band emission in the APOGEE spectra, but two stars classified as B[e] in the literature were observed (ABE-A23 and ABE-A35) as was a reported Herbig Ae star (ABE-A33); Q = Stars which (a) had existing "emission line star" classifications in the literature, (b) appeared to be hot OBA stars in the APOGEE spectra, but (c) did not produce any discernible emission in any of the associated APOGEE data (all have multi-epoch data), or in others words, were H-band quiescent (hence the "Q" of the ABE IDs) during the observations. Note (2): APOGEE is the Apache Point Observatory Galactic Evolution Experiment (APOGEE; Majewski, 2012AAS...21920506M). Note (3): The flag on spectral type is defined as follows: CSSC = The Catalogue of Stellar Spectral Classification (CSSC; Skiff 2013, cat. B/mk) was the primary resource used for locating spectral type information, but some of the original sources of spectral types in the CSSC (primarily those pre-dating 1940) could not be tracked down (in those cases, the spectral types are enclosed in parentheses). Other second-hand spectral types, culled from modern compilations of historical data, are also enclosed in parentheses. Note (4): Mean emission peak velocity separation {Delta}vp measurement could not be made in any of the available spectra despite evidence of emission or shell absorption. In place of a {Delta}vp value, an abbreviation is provided as follows: w = Weak emission-peaks not discernible; w? = Weak or ambiguous detection; sp = Single-peaked emission; sh = Shell absorption without resolved adjacent emission peaks; as = Highly asymmetric emission peaks such that only one is visible (not the same as single-peaked; ABE-056 and ABE- A03); bl = V peak of Br11 is severely blended with FeII 16792 (ABE-013); tc = Spectra are heavily contaminated by telluric features (ABE-058).
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Ref Reference identifier 4- 22 A19 --- BibCode Bibliographic code 24- 45 A22 --- Aut Author's name 47- 70 A24 --- Cat Catalog in VizieR database
History: From electronic version of the journal References: Chojnowski et al., Paper II. 2017AJ....153..174C, Cat. J/AJ/153/174 ================================================================================ (End) Greg Schwarz [AAS], Sylvain Guehenneux [CDS] 29-Jan-2015