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J/ApJ/700/1299       Gas-phase element depletions in the ISM     (Jenkins, 2009)

A unified representation of gas-phase element depletions in the interstellar medium. Jenkins E.B. <Astrophys. J., 700, 1299-1348 (2009)> =2009ApJ...700.1299J
ADC_Keywords: Interstellar medium ; Stars, nearby ; Abundances Keywords: ISM: abundances - ISM: atoms - ultraviolet: ISM Abstract: A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 150 276 Stellar data and line of sight information table4.dat 86 16 Element depletion parameters table5.dat 130 239 Observed and synthetic log N(H) and F* table6.dat 84 29 Synthetic log N(H) and F* for stars in the Local Bubble table7.dat 108 1475 Observations and fits for Carbon - Krypton refs.dat 69 138 References notes.dat 76 44 Notes of table 2
See also: II/114 : UV Interstellar Extinction (Savage+ 1985) II/215 : uvby-beta Catalogue (Hauck+ 1997) III/205 : H-alpha Stars in Northern Milky Way (Kohoutek+ 1997) J/A+A/275/549 : Interstellar extinction curves (Jenniskens+ 1993) J/A+AS/107/385 : UV-excess objects Spacelab-1 survey IV. (Tobin+, 1994) J/ApJS/93/211 : IUE survey of H I Lyα absorption. I. (Diplas+ 1994) J/ApJS/136/631 : IUE absorption toward 164 early-type stars (Savage+, 2001) J/ApJS/146/125 : O VI in the galactic halo (Savage+, 2003) J/ApJS/147/61 : Interstellar Ca I absorption (Welty+, 2003) J/MNRAS/367/1478 : Interstellar NaI, TiII + CaIIK obs. (Hunter+, 2006) J/ApJ/647/328 : FUSE survey of OVI in ISM (Dixon+, 2006) J/ApJS/176/59 : FUSE survey of OVI in the disk of the Milky Way (Bowen+, 2008) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD ? HD number 11- 13 I3 km/s Vcomp ? Specific Heliocentric velocity component 16- 31 A16 --- Name Name (1) 33- 38 F6.2 deg GLON Galactic longitude 40- 45 F6.2 deg GLAT Galactic latitude 47- 51 F5.2 mag Vmag The Simbad V band magnitude (not used for calculating the reddenings or Dist) 53- 68 A16 --- SpType MK spectral type 70- 75 A6 --- r_SpType Reference for SpType; see refs.dat file 77- 81 F5.2 mag E(B-V) The (B-V) extinction 83- 87 F5.3 kpc Dist Heliocentric distance (1) 89- 93 F5.2 kpc Z Distance from Galactic plane 95- 99 F5.2 [cm-2] b_logNHI ? Lower limit on logNHI 103-107 F5.2 [cm-2] logNHI ? Log best observed HI column density 109 A1 --- n_logNHI Flag on logNHI (see notes.dat file) 111-115 F5.2 [cm-2] B_logNHI ? Upper limit on logNHI 119-124 A6 --- r_logNHI Reference for logNHI; see refs.dat file 127-131 F5.2 [cm-2] b_logNH2 ? Lower limit on logNH2 133-137 F5.2 [cm-2] logNH2 ? Log best observed H2 column density 139-143 F5.2 [cm-2] B_logNH2 ? Upper limit on logNH2 145-150 A6 --- r_logNH2 Reference for logNH2; see refs.dat file
Note (1): Stars for which neither the Hipparcos parallaxes (Cat. I/311) nor the determinations by Bowen et al. 2008, Cat. J/ApJS/176/59 were applicable had their spectroscopic parallaxes determined with the standard formula for the distance d (in kpc): logd=(mV-AV-MV-10)/5, where mV is the apparent V magnitude of the star, AV is the extinction by dust in the visible (assumed to be 3.1E(B-V)), and MV is the absolute V magnitude of the star. See section 4.5.1 for further details.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 2 A2 --- El Element identification "X" (1) 4- 7 F4.2 [-] [X/H] Adopted reference abundance relative to H (2) 9- 12 F4.2 [-] e_[X/H] Uncertainty in X/H (2) 14- 19 F6.3 --- Ax The A_X_ parameter; defined in Eq. 10 (3) 21- 25 F5.3 --- e_Ax Uncertainty in Ax 27- 32 F6.3 --- Bx The B_X_ parameter; defined in Eq. 10 (3) 34- 38 F5.3 --- e_Bx Uncertainty in Bx (4) 40- 44 F5.3 --- zx The z_X_ parameter; defined in Eq. 11 (3) 46- 51 F6.3 [-] Xgas/H0 The [Xgas/H]0 parameter; defined in Eq. 13 53- 57 F5.3 [-] e_Xgas/H0 Uncertainty in Xgas/H0; defined in Eq. 14 (3)(4) 59- 64 F6.3 [-] Xgas/H1 The [Xgas/H]1 parameter; defined in Eq. 15 66- 70 F5.3 [-] e_Xgas/H1 Uncertainty in Xgas/H1; defined in Eq. 16 (4) 72- 76 F5.1 --- chi2 The χ2 value 78- 80 I3 --- dof Degrees of freedom 82- 86 F5.3 --- Prob Probability of worse fit
Note (1): Coefficients for S do not appear in this table because a nonstandard approach was required. The coefficients are given in the text of Section 9. Note (2): On a logarithmic scale with H=12. Values and their errors taken from the recommended solar abundances of Lodders K. (2003ApJ...591.1220L). Note (3): The slope of a best-fit line for the observed depletions [Xgas/H]obs=AX(F*-zX)+BX for any given element X against F* (the line-of-sight depletion strength factor). The parameter AX represents the propensity of that element to increase (the absolute value of) its particular depletion level as F* becomes larger. For even the smallest observed values of F*, most elements still show some depletion (see Figure 1). We denote this level of depletion as [Xgas/H]0. See section 3 for further details. Note (4): Unlike the convention for listing errors in the fit outcomes in Table 7, the uncertainties with the terms listed here include both the formal errors of the fit coefficients and the error in the adopted value of (X/H), added together in quadrature.
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD ? HD number 11- 13 I3 km/s Vcomp ? Specific Heliocentric velocity component (1) 16- 31 A16 --- Name Name 33- 37 F5.2 [cm-2] b_logNHo ? Lower limit on logNHOb 39- 43 F5.2 [cm-2] logNHo ? Log observed H column density 45- 49 F5.2 [cm-2] B_logNHo ? Upper limit on logNHOb 51- 55 F5.2 --- F*o ? Observed line-of-sight depletion strength factor 57- 60 F4.2 --- e_F*o ? Uncertainty in F*o 62- 66 F5.2 [cm-2] logNHs ? Log synthetic H column density 68- 71 F4.2 [cm-2] e_logNHs ? Uncertainty in logNHs 73- 77 F5.2 --- F*s ? Synthetic line-of-sight depletion strength factor 79- 82 F4.2 --- e_F*s ? Uncertainty in F*s 84- 88 F5.3 --- Prob ? Probability of a worse fit 90-130 A41 --- El Elements considered in fit
Note (1): Separate velocity components, explicitly identified and not grouped together; see section 4.3.
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 8 A8 --- WD White Dwarf identification (HHMM+DDd; B1950) 10- 24 A15 --- AName Alternate name 26- 31 F6.2 deg GLON Galactic longitude 33- 38 F6.2 deg GLAT Galactic latitude 40- 43 F4.1 mag Vmag The Simbad V band magnitude 45- 47 I3 pc Dist Heliocentric distance (1) 49- 53 F5.2 [-] logNHs Log synthetic H column density 55- 58 F4.2 [-] e_logNHs Uncertainty in logNHs 60- 64 F5.2 --- F*s Synthetic line-of-sight depletion strength factor 66- 69 F4.2 --- e_F*s Uncertainty in F*s 71- 74 F4.2 --- chi2 ? The χ2 value 76- 84 A9 --- El Element(s) considered (2)
Note (1): Taken from the papers that described the FUSE observations. Note (2): All column density data from Lehner et al. (2003ApJ...595..858L), except for HZ 21 (Oliveira et al. 2003ApJ...587..235O).
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 2 A2 --- El Element "X" 4- 9 I6 --- HD ? HD number 12- 14 I3 km/s Vcomp ? Specific Heliocentric velocity component 17- 32 A16 --- Name Name (1) 34- 38 F5.2 [cm-2] b_logNx ? Lower limit on logNx 42- 46 F5.2 [cm-2] logNx ? Log best observed column density (2) 48 A1 --- f_logNx [if] infinite or fixed value of logNx (3) 50- 54 F5.2 [cm-2] B_logNx ? Upper limit on logNx 56 A1 --- n_logNx [if] infinite or fixed value of B_logNx (3) 58- 63 A6 --- r_logNx Reference codes for logNx (see refs.dat file) 65- 69 F5.2 --- F* ? Line-of-sight depletion strength factor 71- 74 F4.2 --- e_F* ? Uncertainty in F* 76- 81 F6.3 [-] [X/H] ? Log expected depletion [X_gas_/H] (4) 83- 87 F5.3 [-] e_[X/H] ? Uncertainty in Elgas/H 89- 94 F6.3 --- Res ? Observed [X/H] minus computed from Eq. 10 96-100 F5.2 --- sigma ? Standard deviation (5)
Note (1): In table 7, ο2 Sco is a misprint for ο1 Sco; corrected at CDS. Note (2): Column densities for CII, NI, OI, MgII, SiII, PII, SII, ClII, TiII, CrII, MnII, FeII, NiII, CuII, ZnII, GeII, and KrI. Note (3): Flag as follows: i = indicates value is infinite; f = The entry 13.44 for the adopted value of N (NiII) stated by CLMS06 (Cartledge et al. 2006ApJ...641..327C) is incorrect; this number should be 13.94, as confirmed by Cartledge (private communication). The value listed here includes a correction for a change in the transition f -value by -0.106dex - see Table 1. Note (4): Computed using Eq. 10. The listed errors do not include an overall systematic uncertainty of C/H = 0.04, N/H = 0.11, O/H = 0.05, Mg/H = 0.02, Si/H = 0.02, P/H = 0.04, S/H = 0.04, Cl/H = 0.06, Ti/H = 0.03, Cr/H = 0.05, Mn/H = 0.03, Fe/H = 0.03, Ni/H = 0.03, Cu/H = 0.06, Zn/H = 0.04, Ge/H = 0.05, and Kr/H = 0.08 in the solar abundance in order to show just the formal error that arises from the uncertainties in location of line of best fit and the value of F*. Note (5): The difference shown in the previous column divided by the expected difference due to the uncertainties in both the measured column density and the coefficients that appear in Eq. 10.
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Ref Code of reference 8- 26 A19 --- BibCode Bibcode 28- 48 A21 --- Auth Author's name(s) 51- 69 A19 --- Comm Comment
Byte-by-byte Description of file: notes.dat
Bytes Format Units Label Explanations
1 A1 --- F [d-r] Flag code 3- 76 A74 --- Note Text of note
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 27-Jul-2011
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