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J/MNRAS/404/1321    TiII in Milky way and Magellanic clouds  (Welty+, 2010)
Interstellar Ti II in the Milky way and Magellanic clouds.
    Welty D.E., Crowther P.A.
   <Mon. Not. R. Astron. Soc., 404, 1321-1348 (2010)>
   =2010MNRAS.404.1321W
ADC_Keywords: Interstellar medium ; Abundances ; Spectroscopy

Keywords: ISM: abundances - ISM: lines and bands - galaxies: ISM -
          Magellanic Clouds

Abstract:
    We discuss several sets of TiII absorption-line data, which probe a
    variety of interstellar environments in our Galaxy and in the
    Magellanic Clouds. Comparisons of high-resolution [full width at
    half-maximum (FWHM)∼1.3-1.5km/s] TiII spectra of Galactic targets with
    corresponding high-resolution spectra of NaI, KI and CaII reveal both
    similarities and differences in the detailed structure of the
    absorption-line profiles - reflecting component-to-component
    differences in the ionization and depletion behaviour of those
    species. Moderate-resolution (FWHM∼3.4-4.5km/s) spectra of more
    heavily reddened Galactic stars provide more extensive information on
    the titanium depletion in colder, denser clouds - where more than 99.9
    per cent of the Ti may be in the dust phase. Moderate-resolution
    (FWHM∼4.5-8.7km/s) spectra of stars in the Magellanic Clouds suggest
    that the titanium depletion is generally much less severe in the Large
    and Small Magellanic Clouds than in our Galaxy [for a given N(Htot),
    E(B-V), or molecular fraction f(H2)]- providing additional evidence
    for differences in depletion patterns in those two lower-metallicity
    galaxies. We briefly discuss possible implications of these results
    for the interpretation of gas-phase abundances in quasi-stellar object
    absorption-line systems and of variations in the D/H ratio in the
    local Galactic interstellar medium.

Description:
    The spectroscopic data collected in this survey were obtained using
    either the Kitt Peak 0.9-m coude feed telescope and echelle
    spectrograph or the ESO/VLT UT2 telescope and UVES spectrograph
    between 1994 Sep and 2004 Dec.

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
tablea1.dat       50      286   Component structures for Galactic sight lines
                              for which high-resolution (FWHM<2km/s) CaII
                              spectra are available
tablea2.dat       58      404  *314 Galactic sight lines for which TiII data
                              (λ3383 equivalent widths and/or
                              column density estimates) are available
notes.dat         95       24   References to tablea2.dat
tablea3.dat       77       82   QSOALS TiII column densities
refs.dat          87       27   References to tablea3.dat

Note on  tablea2.dat: All column densities have been scaled to f(3383)=0.358
   (Morton, 2003ApJS..149..205M).


See also:
 J/ApJS/171/29 : UCSD/Keck damped Lyα abundance database (Prochaska+ 2007)


Byte-by-byte Description of file: tablea1.dat

   Bytes Format Units     Label      Explanations

   1-  8  A8    ---       Star       Star name
  10- 16  A7    ---       Run        Run(s) (1)
  19- 21  F3.1  km/s      e_HV       ? Typical 3σ uncertainties on HV (2)
  24- 25  I2    ---       m_Star     Star Component number
  27- 31  F5.1  km/s      HV         Heliocentric velocity
  33- 36  F4.2  km/s      b          b-value (line width) of TiII
      37  A1    ---       r_b        Fixed value of b (3)
      40  A1    ---       l_NTiII    Limit flag on NTiII (3σ)
  41- 44  F4.1  10+10cm-2 NTiII      TiII column density
      45  A1    ---       n_NTiII    Fixed value of NTiII (3)
      46  A1    ---     l_TiII/CaII  Limit flag on TiII/CaII (3σ)
  47- 50  F4.2  ---       TiII/CaII  ?=- TiII/CaII column density ratio

Note (1): Runs as follows:
    H79 = Hobbs, 1979ApJ...229L.129H
    K94 = 1994 Sep, KPNO/coude (cam 6)
    K95 = 1995 Apr, KPNO/coude (cam 6)
    V00 = 2000 Nov, KPNO/coude (cam 5)
    V03 = 2003 Nov, ESO/VLT (UT2) + UVES
Note (2): Typical 3σ uncertainties for a single component with b=2km/s
     and include both photon noise and continuum placement uncertainties.
Note (3): Notes as follows:
      ] = values were fixed in the fits, but are fairly well determined
      ) = values were fixed in the fits, but are less well determined


Byte-by-byte Description of file: tablea2.dat

   Bytes Format Units      Label     Explanations

   1- 18  A18   ---        Name      Name
  20- 21  I2    ---        Note      Note number, in notes.dat file
      23  A1    ---        l_EW      Limit flag on EW
  24- 28  F5.1  0.1nm      EW        ?=- TiII equivalent width
  30- 33  F4.1  0.1nm      e_EW      ? rms uncertainty on EW
      35  A1    ---        l_N(AOD)  Limit flag on N(AOD)
  36- 40  F5.2  10+10cm-2  N(AOD)    ?=- TiII column density obtained by
                                         integrating the "apparent" optical
                                         depth (AOD) over the line profile
  42- 45  F4.2  10+10cm-2  e_N(AOD)  ? rms uncertainty on N(AOD)
      46  A1    ---        n_N(AOD)  [)] ) if N(AOD) obtained either directly
                                          from the equivalent width
      48  A1    ---        l_Nfit    Limit flag on Nfit
  49- 53  F5.2  10+10cm-2  Nfit      ? TiII column density obtained via a
                                       detailed multi-component fit to the line
                                       profile (1)
  55- 58  F4.2  10+10cm-2  e_Nfit    ? rms uncertainty on Nfit

Note (1): which (in principle) can account for any saturation effects
     (if the b-values are well determined)


Byte-by-byte Description of file: notes.dat

   Bytes Format Units   Label     Explanations

   1-  2  I2    ---     Note      Note number, for data origins
   4- 22  A19   ---     BibCode   Bibcode
  24- 46  A23   ---     Aut       Author's name
  48- 95  A48   ---     Com       Comments


Byte-by-byte Description of file: tablea3.dat

   Bytes Format Units   Label     Explanations

   1- 11  A11   ---     QSO       QSO name
      12  A1    ---     Note      [*] Averaged values (1)
  14- 19  F6.4  ---     z         ?=- Redshift
      21  A1    ---     l_HI      Limit flag on HI
  22- 26  F5.2  ---     HI        ?=- HI column density
      28  A1    ---     l_H2      Limit flag on H2
  29- 33  F5.2  ---     H2        ?=- H2 column density
      35  A1    ---     l_ZnII    Limit flag on ZnII
  36- 40  F5.2  ---     ZnII      ?=- ZnII column density
      42  A1    ---     l_[Zn/H]  Limit flag on [Zn/H]
  43- 47  F5.2  ---     [Zn/H]    ?=- [Zn/H] relative abundance
      49  A1    ---     l_CaII    Limit flag on CaII
  50- 54  F5.2  ---     CaII      ?=- CaII column density
      56  A1    ---     l_TiII    Limit flag on TiII
  57- 61  F5.2  ---     TiII      ?=- TiII column density
      63  A1    ---    l_[Ti/Zn]  Limit flag on [Ti/Zn]
  64- 68  F5.2  ---     [Ti/Zn]   ?=- [Ti/Zn] relative abundance
  70- 77  A8    ---     Ref       References, in refs.dat file

Note (1): The last three entries are for the averages of 27, 13, and 14
     CaII-selected systems seen in lower resolution, lower S/N spectra from
     the Sloan Digital Sky Survey (Wild et al., 2006MNRAS.367..211W).


Byte-by-byte Description of file: refs.dat

   Bytes Format Units   Label     Explanations

   1-  2  I2    ---     Ref       Reference number
   4- 22  A19   ---     BibCode   BibCode
  24- 48  A25   ---     Aut       Author's name
  50- 87  A38   ---     Com       Comments


History:
    From electronic version of the journal
(End)                                      Patricia Vannier [CDS]    20-Nov-2010