J/ApJS/236/36 Ga, Ge, As, Kr, Cd, Sn and Pb column densities (Ritchey+, 2018)
Abundances and depletions of neutron-capture elements in the interstellar
medium.
Ritchey A.M., Federman S.R., Lambert D.L.
<Astrophys. J. Suppl. Ser., 236, 36 (2018)>
=2018ApJS..236...36R 2018ApJS..236...36R
ADC_Keywords: Abundances; Interstellar medium; Ultraviolet; Stars, distances
Keywords: ISM: abundances ; ISM: atoms ;
nuclear reactions, nucleosynthesis, abundances ; ultraviolet: ISM
Abstract:
We present an extensive analysis of the gas-phase abundances and
depletion behaviors of neutron-capture elements in the interstellar
medium (ISM). Column densities (or upper limits to the column
densities) of Ga II, Ge II, As II, Kr I, Cd II, Sn II, and Pb II are
determined for a sample of 69 sight lines with high- and/or
medium-resolution archival spectra obtained with the Space Telescope
Imaging Spectrograph (STIS) on board the Hubble Space Telescope. An
additional 59 sight lines with column density measurements reported in
the literature are included in our analysis. Parameters that
characterize the depletion trends of the elements are derived
according to the methodology developed by Jenkins (2009,
J/ApJ/700/1299). The depletion patterns exhibited by Ga and Ge comport
with expectations based on the depletion results obtained for many
other elements. Arsenic exhibits much less depletion than expected,
and its abundance in low-depletion sight lines may even be supersolar.
We confirm a previous finding by Jenkins that the depletion of Kr
increases as the overall depletion level increases from one sight line
to another. Cadmium shows no such evidence of increasing depletion. We
find a significant amount of scatter in the gas-phase abundances of Sn
and Pb. For Sn, at least, the scatter may be evidence of real
intrinsic abundance variations due to s-process enrichment combined
with inefficient mixing in the ISM.
Description:
The primary aim of our extensive search of the HST/Space Telescope
Imaging Spectrograph (STIS) archive was the identification of sight
lines showing significant absorption from AsIIλ1263,
CdIIλ2145, SnIIλ1400, and PbIIλ1433.
In addition to searching for absorption from As II, Cd II, Sn II, and
Pb II, we sought to incorporate available data on GaII, GeII, and KrI
into our analysis so that the abundances of all seven n-capture
elements could be analyzed in a consistent manner.
We also examined the HST/Goddard High-Resolution Spectrograph (GHRS)
data on GeIIλ1237, along with STIS data for the weaker GeII
line at 1602.5λ.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 85 69 Stellar data
table4.dat 61 62 Component structure
table5.dat 168 69 Column densities
table7.dat 184 52 Elemental abundances
table8.dat 87 8 Element depletion parameters
table11.dat 166 60 Column densities obtained from the literature
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See also:
B/hst : HST Archived Exposures Catalog (STScI, 2007)
I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007)
J/ApJS/93/211 : IUE survey of H I Lyα absorption. I. (Diplas+ 1994)
J/A+A/334/987 : 6 blue objects spectral data (Venn+ 1998)
J/ApJS/176/59 : FUSE survey of OVI in the disk of the Milky Way (Bowen+, 2008)
J/ApJ/700/1299 : Gas-phase element depletions in the ISM (Jenkins, 2009)
J/MNRAS/418/284 : s-process in low-metallicity stars. II. (Bisterzo+, 2011)
J/ApJ/728/70 : The abundance of boron in diffuse clouds (Ritchey+, 2011)
J/ApJ/787/10 : Solar s-process contributions with GCE model (Bisterzo+, 2014)
J/ApJ/797/69 : Abundances of late-type stars (Roederer+, 2014)
J/ApJS/218/25 : Abundances in PNe. III: Se and Kr (Sterling+, 2015)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Star name
13- 23 A11 --- OName Other name
25- 38 A14 --- SpT MK spectral type
40 I1 --- r_SpT [1/8] Reference (1)
42- 46 F5.2 mag Vmag V-band magnitude from SIMBAD
47 A1 --- n_Vmag Flag on Vmag (2)
49- 52 F4.2 mag E(B-V) Color excess (3)
53 A1 --- n_E(B-V) Flag on E(B-V) (2)
55- 60 F6.2 deg GLON [1.6/359] Galactic longitude from SIMBAD
62- 67 F6.2 deg GLAT [-28.2/56] Galactic latitude from SIMBAD
69- 73 F5.2 kpc Dist [0.1/27] Distance (3)
75- 78 F4.2 kpc e_Dist ? Distance uncertainty
79 A1 --- n_Dist Flag on Dist (2)
81- 85 F5.2 kpc Z [-3.2/3.2] Z distance (see section 2.2)
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Note (1): Reference as follows:
1 = Jenkins, 2009, J/ApJ/700/1299
2 = Houk & Cowley (1975mcts.book.....H 1975mcts.book.....H)
3 = Bowen et al. 2008, J/ApJS/176/59
4 = Houk & Smith-Moore (1988mcts.book.....H 1988mcts.book.....H)
5 = Sota et al. (2014, III/274)
6 = Hill (1970MNRAS.150...23H 1970MNRAS.150...23H)
7 = Simonson (1968ApJ...154..923S 1968ApJ...154..923S)
8 = Venn et al. (1998, J/A+A/334/987)
Note (2): Note as follows:
b = These values of E(B-V) and Dist were derived following the set of
procedures outlined in Appendix B of B08 (Bowen+, 2008, J/ApJS/176/59),
using intrinsic colors from Wegner (1994MNRAS.270..229W 1994MNRAS.270..229W) and absolute
visual magnitudes from B08.
c = These values of E(B-V) and Dist were obtained directly from Table 1 of
B08 (Bowen+, 2008, J/ApJS/176/59).
d = The apparent V-band magnitude of this star is dominated by the cool
component, which has V=5.71 (based on a transformation of the Tycho
magnitudes for this component; ESA 1997, I/239). The hot component has
V=9.24 and is the one used to calculate the distance of 1.4kpc.
Note (3): Values of E(B-V) and Dist are mainly from J09
(Jenkins, 2009, J/ApJ/700/1299).
Distances with error bars are from ≥4σ Hipparcos results
(van Leeuwen 2007, I/311). Other exceptions are noted.
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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- 11 A11 --- Name Star name
13- 17 F5.1 km/s OI-vlsr [-53/9.3]? LSR velocity, OI 1355Å
19- 21 F3.1 km/s OI-b [0.5/4.4]? Doppler parameter, b, OI 1355Å
23- 26 F4.2 --- OI-N/Ntot ? Fractional column density, OI 1355Å
28- 32 F5.1 km/s GaII-vlsr [-52.6/8.7]? LSR velocity, GaII 1414Å
34- 36 F3.1 km/s GaII-b [0.5/4.4]? Doppler parameter, b, GaII 1414Å
38- 41 F4.2 --- GaII-N/Ntot ? Fractional column density, GaII 1414Å
43- 47 F5.1 km/s GeII-vlsr [-57/10.6]? LSR velocity, GeII 1237Å
49- 51 F3.1 km/s GeII-b [0.5/4.3]? Doppler parameter, b, GeII 1237Å
53- 56 F4.2 --- GeII-N/Ntot ? Fractional column density, GeII 1237Å
59- 61 A3 --- Notes Notes (1)
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Note (1): Notes as follows:
1 = Derived from medium-resolution (E140M) data;
2 = Derived from high-resolution (E140H) data;
3 = No GaII data are available.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Star name
13- 18 F6.3 [cm-2] logN(OI) [17.1/18.4] log10 OI column density
20- 24 F5.3 [cm-2] E_logN(OI) [0.003/0.1] Upper uncertainty in logN(OI)
26- 30 F5.3 [cm-2] e_logN(OI) [0.004/0.2] Lower uncertainty in logN(OI)
32- 32 A1 --- f_logN(OI) Flag on logN(OI) (1)
34- 34 A1 --- l_logN(GaII) Limit flag on logN(GaII)
36- 40 F5.2 [cm-2] logN(GaII) [10.7/12.1]? log10 GaII column density
42- 45 F4.2 [cm-2] E_logN(GaII) [0.01/0.2]? Upper uncertainty in logN(GaII)
47- 50 F4.2 [cm-2] e_logN(GaII) [0.01/0.3]? Lower uncertainty in logN(GaII)
52- 52 A1 --- f_logN(GaII) Flag on logN(GaII) (1)
54- 58 F5.2 [cm-2] logN(GeII) [11.5/13]? log10 GeII column density
60- 63 F4.2 [cm-2] E_logN(GeII) [0.02/0.2]? Upper uncertainty in logN(GeII)
65- 68 F4.2 [cm-2] e_logN(GeII) [0.02/0.2]? Lower uncertainty in logN(GeII)
70- 70 A1 --- f_logN(GeII) Flag on logN(GeII) (1)
72- 72 A1 --- l_logN(AsII) Limit flag on logN(AsII)
74- 78 F5.2 [cm-2] logN(AsII) [11.3/12.5]? log10 AsII column density
80- 83 F4.2 [cm-2] E_logN(AsII) [0.05/0.2]? Upper uncertainty in logN(AsII)
85- 88 F4.2 [cm-2] e_logN(AsII) [0.05/0.3]? Lower uncertainty in logN(AsII)
90- 90 A1 --- f_logN(AsII) Flag on logN(AsII) (1)
92- 92 A1 --- l_logN(KrI) Limit flag on logN(KrI)
94- 98 F5.2 [cm-2] logN(KrI) [11.5/13.4]? log10 KrI column density
100-103 F4.2 [cm-2] E_logN(KrI) [0.01/0.2]? Upper uncertainty in logN(KrI)
105-108 F4.2 [cm-2] e_logN(KrI) [0.01/0.2]? Lower uncertainty in logN(KrI)
110-110 A1 --- f_logN(KrI) Flag on logN(KrI) (1)
112-112 A1 --- l_logN(CdII) Limit flag on logN(CdII)
114-118 F5.2 [cm-2] logN(CdII) [10.9/12]? log10 CdII column density
120-123 F4.2 [cm-2] E_logN(CdII) [0.02/0.2]? Upper uncertainty in logN(CdII)
125-128 F4.2 [cm-2] e_logN(CdII) [0.03/0.2]? Lower uncertainty in logN(CdII)
130-130 A1 --- f_logN(CdII) Flag on logN(CdII) (1)
132-132 A1 --- l_logN(SnII) Limit flag on logN(SnII)
134-138 F5.2 [cm-2] logN(SnII) [10.8/12]? log10 SnII column density
140-143 F4.2 [cm-2] E_logN(SnII) [0.01/0.2]? Upper uncertainty in logN(SnII)
145-148 F4.2 [cm-2] e_logN(SnII) [0.01/0.3]? Lower uncertainty in logN(SnII)
150-150 A1 --- l_logN(PbII) Limit flag on logN(PbII)
152-156 F5.2 [cm-2] logN(PbII) [11/12.2]? log10 PbII column density
158-161 F4.2 [cm-2] E_logN(PbII) [0.06/0.2]? Upper uncertainty in logN(PbII)
163-166 F4.2 [cm-2] e_logN(PbII) [0.07/0.3]? Lower uncertainty in logN(PbII)
168-168 A1 --- f_logN(PbII) Flag on logN(PbII) (1)
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Note (1): Flags as follows:
a = Weighted mean of the column densities obtained from high-resolution
(E140H) and medium-resolution (E140M) data;
b = Column density obtained from the PbII 1203A line;
c = Weighted mean of the column densities obtained from the GeII 1237A
line (from GHRS data) and the GeII 1602A line (from STIS data);
d = Column density obtained from the KrI 1164A line from FUSE data;
e = Weighted mean of the column densities obtained from the CdII 2145A
and 2265A lines.
f = The expected position of the AsII 1263A line overlaps with a
high-velocity component of SiII* 1264A, precluding a detection of
AsII in this direction.
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Star name
13- 17 F5.2 [cm-2] logN(Htot) [20.5/21.8] log10 total hydrogen column
density (G1)
19- 22 F4.2 [cm-2] E_logN(Htot) [0.02/0.2] Upper uncertainty for logN(Htot)
24- 27 F4.2 [cm-2] e_logN(Htot) [0.02/0.2] Lower uncertainty for logN(Htot)
29- 29 A1 --- f_logN(Htot) Flag on logN(Htot) (1)
31- 34 F4.2 --- F* [0.1/1]? Line-of-sight depletion factor (G1)
36- 39 F4.2 --- e_F* [0.02/0.5]? Uncertainty in F*
41- 41 A1 --- f_F* Flag on F* (1)
43- 47 F5.2 [-] log(O/H) [-3.6/-3.1]? log10 O/H abundance
49- 52 F4.2 [-] E_log(O/H) [0.03/0.2]? Upper uncertainty for log(O/H)
54- 57 F4.2 [-] e_log(O/H) [0.04/0.2]? Lower uncertainty for log(O/H)
59- 64 F6.2 [-] log(Ga/H) [-10.2/-9.3]? log10 Ga/H abundance
66- 69 F4.2 [-] E_log(Ga/H) [0.03/0.2]? Upper uncertainty for log(Ga/H)
71- 74 F4.2 [-] e_log(Ga/H) [0.04/0.2]? Lower uncertainty for log(Ga/H)
76- 80 F5.2 [-] log(Ge/H) [-9.3/-8.5]? log10 Ge/H abundance
82- 85 F4.2 [-] E_log(Ge/H) [0.04/0.2]? Upper uncertainty for log(Ge/H)
87- 90 F4.2 [-] e_log(Ge/H) [0.05/0.2]? Lower uncertainty for log(Ge/H)
92- 92 A1 --- l_log(As/H) Limit flag on log(As/H)
94- 99 F6.2 [-] log(As/H) [-10.1/-8.9]? log10 As/H abundance
101-104 F4.2 [-] E_log(As/H) [0.07/0.2]? Upper uncertainty for log(As/H)
106-109 F4.2 [-] e_log(As/H) [0.08/0.4]? Lower uncertainty for log(As/H)
111-111 A1 --- l_log(Kr/H) Limit flag on log(Q/H)
113-117 F5.2 [-] log(Kr/H) [-9.2/-8.1]? log10 Kr/H abundance
119-122 F4.2 [-] E_log(Kr/H) [0.06/0.2]? Upper uncertainty for log(Kr/H)
124-127 F4.2 [-] e_log(Kr/H) [0.06/0.2]? Lower uncertainty for log(Kr/H)
129-129 A1 --- l_log(Cd/H) Limit flag on log(Cd/H)
131-136 F6.2 [-] log(Cd/H) [-10.6/-9.8]? log10 Cd/H abundance
138-141 F4.2 [-] E_log(Cd/H) [0.05/0.2]? Upper uncertainty for log(Cd/H)
143-146 F4.2 [-] e_log(Cd/H) [0.05/0.3]? Lower uncertainty for log(Cd/H)
148-148 A1 --- l_log(Sn/H) Limit flag on log(Sn/H)
150-155 F6.2 [-] log(Sn/H) [-10.4/-9]? log10 Sn/H abundance
157-160 F4.2 [-] E_log(Sn/H) [0.04/0.2]? Upper uncertainty for log(Sn/H)
162-165 F4.2 [-] e_log(Sn/H) [0.04/0.3]? Lower uncertainty for log(Sn/H)
167-167 A1 --- l_log(Pb/H) Limit flag on log(Pb/H)
169-174 F6.2 [-] log(Pb/H) [-10.3/-8.9]? log10 Pb/H abundance
176-179 F4.2 [-] E_log(Pb/H) [0.07/0.2]? Upper uncertainty for log(Pb/H)
181-184 F4.2 [-] e_log(Pb/H) [0.08/0.3]? Lower uncertainty for log(Pb/H)
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Note (1): Flags on individual source measurements as follows:
b = The large correction for stellar Lyα contamination applied to
N(HI) for this star by J09 (Jenkins, 2009, J/ApJ/700/1299) may not be
necessary. Here, we adopt the uncorrected value of N(HI) from
Cartledge+ (2004ApJ...613.1037C 2004ApJ...613.1037C). This sight line is not used in the
depletion analysis.
c = Measurement of N(H2) is not available. However, the weak or absent
absorption from ClI 1347A indicates that there is very little H2 in
the line of sight, and we adopt N(HI) (from Jenkins,
2009, J/ApJ/700/1299) as representative of N(Htot). The sight line is
not included in the depletion analysis.
d = This star is not listed in J09 (Jenkins, 2009, J/ApJ/700/1299); the
total hydrogen column density was calculated using N(HI) from
Diplas & Savage (1994, J/ApJS/93/211) and N(H2) from
Sheffer+ (2007ApJ...667.1002S 2007ApJ...667.1002S).
e = The value of N(HI) for this star is listed incorrectly in J09. Here,
we adopt the correct value from Diplas & Savage (1994, J/ApJS/93/211),
and provide an updated value for the sight-line depletion factor F*
(E. Jenkins 2012, private communication).
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- El Element
4- 9 F6.2 [Sun] log(X/H)s [-10.2/-3.2] log10 solar reference
abundance (1)
11- 14 F4.2 [Sun] e_log(X/H)s [0.03/0.08] Uncertainty in log(X/H)s
16- 21 F6.3 --- Ax [-1.1/-0.02] Depletion slope, AX,
as defined in Equation 1 (2)
23- 27 F5.3 --- e_Ax [0.04/0.4] Uncertainty in Ax
29- 34 F6.3 --- Bx [-1/-0.1] Depletion intercept, BX,
as defined in Equation 1 (2)
36- 40 F5.3 --- e_Bx [0.04/0.09] Uncertainty in Bx
42- 46 F5.3 --- zx [0.6/0.9] Depletion parameter, zX,
as defined in Equation 11 of
J09 (Jenkins, 2009, J/ApJ/700/1299)
48- 53 F6.3 --- [X/H]0 [-0.5/0.8] Depletion at F*=0 as defined
in Equation 2 (3)
55- 59 F5.3 --- e_[X/H]0 [0.05/0.4] Uncertainty in [X/H]0
61- 66 F6.3 --- [X/H]1 [-1.3/-0.1] Depletion at F*=1 as defined
in Equation 3 (4)
68- 72 F5.3 --- e_[X/H]1 [0.04/0.1] Uncertainty in [X/H]1
74- 77 F4.1 --- chi2 [6.8/89.6] χ^2 value
79- 80 I2 --- dof [7/89] Degrees of freedom in the fit
82- 82 A1 --- l_Prob Limit flag on Prob
83- 87 F5.3 --- Prob Probability of worse fit
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Note (1): Recommended solar system abundances from Lodders (2003ApJ...591.1220L 2003ApJ...591.1220L)
Note (2): In an idealized situation, the depletion of element X, defined in
logarithmic terms as [X/H]=log(X/H)-log(X/H)☉, is related to
the sight-line depletion factor F* according to Equation (1):
[X/H]=BX+AX(F*-zX) where the depletion parameters, AX, BX,
and zX, are unique to element X.
Note (3): Equation (2): [X/H]0=BX-AXzX (see section 4.2.3).
Note (4): Equation (3): [X/H]1=BX+AX(1-zX) (see section 4.2.3).
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Byte-by-byte Description of file: table11.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Star name
13- 25 A13 --- OName Other Name
27- 31 F5.2 [cm-2] logN(Htot) [20/21.7]? log10 total hydrogen
column density (G1)
33- 36 F4.2 [cm-2] E_logN(Htot) [0.03/0.2]? Upper uncertainty for logN(Htot)
38- 41 F4.2 [cm-2] e_logN(Htot) [0.03/0.3]? Lower uncertainty for logN(Htot)
43- 43 A1 --- f_logN(Htot) Flag on logN(Htot) (1)
45- 49 F5.2 --- F* [0/1.3]? Line-of-sight depletion factor (G1)
51- 54 F4.2 --- e_F* [0.02/0.6]? Uncertainty in F*
56- 60 F5.2 [cm-2] logN(OI) [16.6/18.2]? log10 OI column density
62- 65 F4.2 [cm-2] e_logN(OI) [0.02/0.2]? Uncertainty in logN(OI)
67- 67 A1 --- f_logN(OI) Flag on logN(OI) (1)
69- 73 F5.2 [cm-2] logN(GaII) [10.8/11.7]? log10 GaII column density
75- 78 F4.2 [cm-2] e_logN(GaII) [0.02/0.2]? Uncertainty in logN(GaII)
80- 84 F5.2 [cm-2] logN(GeII) [11.5/12.6]? log10 GeII column density
86- 89 F4.2 [cm-2] e_logN(GeII) [0.02/0.1]? Uncertainty in logN(GeII)
91- 95 F5.2 [cm-2] logN(AsII) [11/11.6]? log10 AsII column density
97-100 F4.2 [cm-2] e_logN(AsII) [0.09/0.2]? Uncertainty in logN(AsII)
102-106 F5.2 [cm-2] logN(KrI) [11.4/12.7]? log10 KrI column density
108-111 F4.2 [cm-2] e_logN(KrI) [0.03/0.2]? Uncertainty in logN(KrI)
113-113 A1 --- f_logN(KrI) Flag on logN(KrI) (1)
115-119 F5.2 [cm-2] logN(CdII) [10/11]? log10 CdII column density
121-124 F4.2 [cm-2] e_logN(CdII) [0.1/0.2]? Uncertainty in logN(CdII)
126-130 F5.2 [cm-2] logN(SnII) [10.5/11.5]? log10 SnII column density
132-135 F4.2 [cm-2] e_logN(SnII) [0.03/0.2]? Uncertainty in logN(SnII)
137-137 A1 --- f_logN(SnII) Flag on logN(SnII) (1)
139-143 F5.2 [cm-2] logN(PbII) [10.7/11]? log10 PbII column density
145-148 F4.2 [cm-2] e_logN(PbII) [0.1/0.2]? Uncertainty in logN(PbII)
150-166 A17 --- Ref References (2)
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Note (1): Flags as follows:
b = The OI and SnII column densities listed here for ζ Per are from
GHRS observations (Meyer+ 1998ApJ...493..222M 1998ApJ...493..222M ;
Sofia+ 1999ApJ...522L.137S 1999ApJ...522L.137S) and are not used in the depletion analysis.
We use the values we obtain from STIS observations instead (see Table5).
The GHRS result for KrI listed here (from Cardelli & Meyer
1997ApJ...477L..57C 1997ApJ...477L..57C) is used in the analysis, however, because the
STIS observations do not cover the KrI 1235Å line.
c = This sight line has an OI column density from Copernicus observations
(Meyer+ 1998ApJ...493..222M 1998ApJ...493..222M), which is not used in the
depletion analysis. We restrict our analysis of O abundances to sight
lines with column density measurements from STIS or GHRS observations.
d = The large correction for stellar Lyα contamination applied to
N(HI) for this star by J09 may not be necessary. Here, we adopt the
uncorrected value of N(HI) from Cartledge+ (2004ApJ...613.1037C 2004ApJ...613.1037C).
This sight line is not used in the depletion analysis.
Note (2): References as follows:
1 = Meyer et al. (1998ApJ...493..222M 1998ApJ...493..222M);
2 = Cartledge et al. (2004ApJ...613.1037C 2004ApJ...613.1037C);
3 = Cartledge et al. (2006ApJ...641..327C 2006ApJ...641..327C);
4 = Cartledge et al. (2008ApJ...687.1043C 2008ApJ...687.1043C);
5 = Cardelli & Meyer (1997ApJ...477L..57C 1997ApJ...477L..57C);
6 = Sofia et al. (1999ApJ...522L.137S 1999ApJ...522L.137S);
7 = Welty et al. (1999ApJS..124..465W 1999ApJS..124..465W);
8 = Cartledge et al. (2003ApJ...597..408C 2003ApJ...597..408C);
9 = Hobbs et al. (1993ApJ...411..750H 1993ApJ...411..750H);
10 = Andre et al. (2003ApJ...591.1000A 2003ApJ...591.1000A);
11 = Welty et al. (1995ApJ...449L.135W 1995ApJ...449L.135W);
12 = Federman et al. (2003ApJ...591..986F 2003ApJ...591..986F);
13 = Savage et al. (1992ApJ...401..706S 1992ApJ...401..706S);
14 = Cardelli et al. (1993ApJ...416L..41C 1993ApJ...416L..41C);
15 = Cardelli (1994Sci...265..209C 1994Sci...265..209C);
16 = Snow et al. (1996ApJ...465..245S 1996ApJ...465..245S);
17 = Cartledge et al. (2001ApJ...562..394C 2001ApJ...562..394C);
18 = Welty (2007ApJ...668.1012W 2007ApJ...668.1012W).
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Global notes:
Note (G1): Total hydrogen column densities were calculated from the values of
N(HI) and N(H2) listed in J09 (Jenkins, 2009, J/ApJ/700/1299), unless
otherwise noted. The line-of-sight depletion factors F* are the observed
values from J09.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 30-Aug-2018