- update Fe II files, add HCl, HF and SiO to hydride files, Septemper 2019
- corrected the Sc II files, November 12 2018
- corrected the Kurucz Co I hfs file, July 29, 2018
- added new Co II lab data, and published lab data for mostly neutron-capture species lines (mostly in the UV) employed in recent papers by Ian Roederer, March 17 2018
- update for Fe I, October 28 2017
- Vini Placco & Chris Sneden, July 18 2017
- Ian Roederer & Vini Placco, & Chris Sneden, Dec 7 2017
SOURCES OF GF'S, HFS/ISO, AND OTHER COMMENTS
UPDATED SEPTEMBER 2019: ADDED HF and HCl FROM THE HITRAN DATABASE
UPDATED JUNE 2019: ADDED FE II FROM THE NEW DEN HARTOG PAPER.
UPDATED MARCH 2018; THESE LINE LISTS ARE CONSERVATIVE IN THE SENSE THAT THEY DO NOT INCLUDE DATA FOR SOME SPECIES THAT MIGHT BE PRETTY GOOD BUT ARE IN NEED OF NEW LAB WORK, SUCH AS NI II AND CO II.
NOTE THAT THE LINEMAKE COMMANDS ARE SET TO WORK ON THE DATA FILES INCLUDED HERE. IF YOU DESIRE TO ADD IN YOUR OWN CHOSEN LINE LISTS TO THIS MIX, THEN: (a) YOU ARE ON YOUR OWN (!); and (b) PLEASE CONTACT ONE OF US ON HOW TO CORRECTLY MERGE YOUR DATA SET WITH OURS.
The linemake code produces MOOG-compatible synthesis line list by starting with the Kurucz compendium (http://kurucz.harvard.edu/linelists.html) and then substituting, adding, splitting, etc., these lists to employ the excellent atomic data from the Wisconsin group (Jim Lawler and associates) and excellent molecular data from the Old Dominion group (Peter Bernath and associates). The only manual steps in getting the code to work are editing lines 19-20 to put the code path into the code, and compiling with f77, g77, or gfortran.
The maximum ionization state is the first ion, and the maximum lower excitation enrgy is 7.5eV except for some light neutral species (neuatrals and ions of these atoms: H, C, N, O, Mg, Al, Si, P, S) for which higher excitation species are considered, and for Fe II, where 8.5eV is the maximum lower energy.
Obvious warnings should be given about the output line lists: we think that they are correct but there is no substitute for you having a close look to assure yourself of their quality. One thing you can do if you are unsure about a line list is to look at the individual files for different species that are sitting in the mooglists subdirectory.
Be really careful about saying yes to the last question when running linemake. This question asks whether or not to add in Kurucz hfs data for transitions of Fe-group elements not done, or yet to be done, by the Wisconsin group. You'll probably get a lot of stuff added into the output line lists, and the pedigrees of these things are not guaranteed.
One oddity that we don't think is worth fixing at the moment: the code does
not work properly when the requested beginning and ending wavelengths bridge the
divide between two files of atomic line data, each of which covers 1000A.
So if you have a desired line list from say 5990A to 6010A, the code screws up.
The work-around simply is to run the code twice, in the example case from 5990A to 5999.999A, and from 6000A to 6010A.
ATOMIC SPECIES: NEUTRON-CAPTURE ELEMENTS (LISTED IN ORDER OF ATOMIC NUMBER)
As I: Roederer & Lawler (2012, ApJ, 750, 76)
Se I: Roederer & Lawler (2012, ApJ, 750, 76)
Rb I: NIST
Sr I: NIST
Sr II: NIST
Y II: Hannaford et al. (1982, ApJ, 261, 736) Biemont et al. (2011, MNRAS, 414, 3350)
Zr II: Ljung et al. (2006, A&A, 456, 1181); Malcheva et al. 2006, MNRAS, 367, 754) for some lines
AgI: Hansen et al. (2012, A&A, 545, 31)
CdI: Morton (2000, ApJS, 130, 403)
Cd II: Roederer & Lawler (2012, ApJ, 750, 76)
Te I: Roederer et al. (2012, ApJL, 747, L8)
La II: Lawler et al. (2001, ApJ, 556, 452)
Ce II: Lawler et al. (2009, ApJS, 182, 51)
Pr II: Sneden et al. (2009, ApJS, 182, 80)
Nd II: Den Hartog et al. (2003, ApJS, 148, 543) Roederer et al. 2008, ApJ, 675, 723 for iso & hfs note that the 4314.50 A line has a solar-derived log(gf)
Sm II: Lawler et al. (2006, ApJS, 162, 227); Roederer & Lawler (2012, ApJ, 750, 76)
Eu II: Lawler et al. (2001, ApJ, 563, 1075)
Gd II: Den Hartog et al. (2006, ApJS, 167, 292)
Tb II: Lawler et al. (2001, ApJS, 137, 341)
Dy II: Sneden et al. (2009, ApJS, 182, 80)
Ho II: Lawler et al. (2004, ApJ, 604, 850)
Er II: Lawler et al. (2008, ApJS, 178, 71)
Tm II: Sneden et al. (2009, ApJS, 182, 80)
Yb II: Sneden et al. (2009, ApJS, 182, 80); DREAM (2116A); Kedzierski et al. (2010, Spectrochem Acta B., 65, 248 2126A); Roederer & Lawler (2012, ApJ, 750, 76)
Lu II: Sneden et al. (2009, ApJS, 182, 80); Roederer et al. (2010, ApJL, 714, L123) for UV log(gf); Roederer et al. (2012, ApJS, 203, 27) for UV hfs
Hf II: Lawler et al. (2007, ApJS, 169, 120)
Pt I: Den Hartog et al. (2005, ApJ, 619, 639); Roederer & Lawler (2012, ApJ, 750, 76)
Hg II: Roederer & Lawler (2012, ApJ, 750, 76) for iso & hfs
Pb I: Biemont et al. (2000, MNRAS, 312, 116) for log(gf); Roederer et al. (2012, ApJS, 203, 27) for iso & hfs
ATOMIC SPECIES: FE-GROUP ELEMENTS (LISTED IN ORDER OF ATOMIC NUMBER)
Sc I: Lawler et al. (2019, ApJS, 241, 21); includes hfs
Sc II: Lawler et al. (2019, ApJS, 241, 21); includes hfs
Ti I: Lawler et al. (2013, ApJS, 205, 11)
Ti II: Wood et al. (2013, ApJS, 208, 27)
V I: Wood et al. (2018, ApJS, 234, 25); Lawler et al. (2014, ApjS, 215, 20); Holmes, C. E. et al. 2016, ApJS, 224, 35 suggested some problems with these transition probabilities in the wavelength range >9000 A, but Wood et al. showed that the Lawler et al. gf's are correct; Wood et al. also has extensive new hfs data.
V II: Wood et al. (2014, ApJS, 214, 18); there is additionaal hfs information in the Kurucz database, collected in vI.kurhfs
Cr I: Sobeck et al. (2007, ApJ, 667, 1267); the line wavelengths have been adjusted to conform to those given at the NIST website
Cr II: Lawler et al. (2017, ApJS, 228, 10).
Mn I: Den Hartog et al. (2011, ApJS, 194, 35); there is additionaal hfs information in the Kurucz database, collected in scI.kurhfs
Mn II: Den Hartog et al. (2011, ApJS, 194, 35); there is no additionl hfs information in the Kurucz database
Fe I: recent lab studies are by Ruffoni et al. (2014, MNRAS, 441, 3127)
Den Hartog (2014, ApJS, 215, 23), and Belmonte et al. (2017, ApJ, 848, 126).
Thefirst two of these papers deal with lines arising (in absorption) from levels with E.P. >~ 2.3 eV. One of the good things about the last paper is that it overlaps the older-but-still-mostly-reliable study of O'Brian et al. (1991, JOSAB, 8, 1185) for lower-excitation transitions.
Here I have chosen to adopt the new lab values, and have added in the O'Brian values not included in the Belmonte paper AND with E.P < 2.2 eV. I consider this list to be as close to an "internally consistent single source" as we are likely to get for a while.
Fe II: Den Hartog et al. (2019, ApJS, 243, 33); most of the new lab data are for UV lines, but enough blue lines (10 of them) are included that it is clear that the Melendez & Barbuy (2009, A&A, 497, 611) empirical values wre more reliable than those at the NIST website. Our choice here is to use the Den Hartog values when available, otherwise to use the Melendez & Barbuy values.
Co I: Lawler et al. (2015, ApJS, 220, 13); Co I with and without hfs are in different files here.
Co II: Lawler et al. (2018, ApJS, 238, 7); there are 12 lines in this paper with good lab hfs patterns. To these we have added another 4 lines with new gf values but approximate hfs patters from the Co I paper; these appear with the notations LAW??? in a linelist generated by linemake.
Ni I: Wood et al. (2014, ApJS, 211, 20); there is isotopic information in the file niI.moogiso, but this is not part of the autometed linemake procedure; one can manually substitute in the relevant structures into a line list.
Ni II: discussed in the Ni I paper, but awaits a fresh study; not included here; this will be the subject of a future Wisconsin lab effort; note that Co II lines in the Kurucz database have no hfs information.
Cu I: not done recently, so any hfs information is not to be trusted much, although for Cu I it is collected in cuI.kurhfs
Zn I: Roederer & Lawler (2012, ApJ, 750, 7Z)
Zn II: Bergeson & Lawler (1993, ApJ, 408, 382)
ATOMIC SPECIES: OTHER ELEMENTS
Li I resonance line: nothing special needs to be done here to get the full isotopic and hyperfine substructure. The total gf from Kurucz, has been adopted; it is close to that recommended by NIST.
MgH: Hinkle et al. (2013, ApJS, 207, 26)
C2 Swan: Ram et al. (2014, ApJS, 211, 5); note that 0.089eV has been added to all of the excitation energies to account for the fact that the lower vibrational level of the Swan system is not exactly at the lowest possible vibrational state.
CN violet and red: Sneden et al. (2014, ApJS, 214, 26)
CO: Pretty much the relatively simply CO parameters in the IR ro-vibrational bands have been known for a couple of decades. However, in trial syntheses conducted by Chris Sneden and Melike Afsar it was noticed that that K-band elta-v = 2 "first overtone" band strengths were too strong for the C and O abundances derived from optical data. But they also clashed with the H-band delta-v = 3 "second overtone" bands in similar fashion. Therefore we decided to raise the gf-values of the delta-v = 2 lines by 0.15 dex, and leave the delta-v = 3 lines alone. This small alteration is in the CO line list here.
OH ro-vibrational bands: Brooke et al. (2015, JQSRT, 168, 142)
HCl: HITRAN database (https://hitran.org/lbl/); IR transitions only
HF: HITRAN database (https://hitran.org/lbl/); IR transitions only
SiO: I added in the Kurucz data for SiO in the IR