OTELO - Spectral Line summary

Registered line list:
Wavelenghts are air wavelenghts.
Values z_min and z_max assume Red OTELO configuration (l.o. min 8980 A and l.o. max 9070 A)
HII, AGN and SNR columns: relative intensities respect to Hβ (=100)

Source Line reference:

(a) SDSS emision line list http://classic.sdss.org/dr6/algorithms/linestable.html
(b) Orion Emission ines from The Orion Complex: A case Study of Interstellar matter by C.D. Goudis 1982, Astrophysics & Space Science Library Vol. 90
(c) An Introduction to Active Galactic Nuclei by Peterson 1997, Cam. Univ. Press
(d) Astrophysics of gaseous nebulae and active galactic nuclei by Osterbrock & Ferland 2006 University Science Books, (2nd Edition); HII, AGN (Cyg A), and SNR; data from SNR: maximun form Crab Nebulae and Cygnus Loop)
(e) From line ID templates for PN by Karen B. Kwitter & Richard B.C. Henry at http://web.williams.edu/Astronomy/research/PN/nebulae/index.php
(f) Form Fanelli, M. N., O'Connell, R.W., Burstein D., Wu, C-C, 1992, ApJSS, 82, 197 and Maraston et al. 2009, A&A 493,425
(g) From Shull, J. M., Stevans, M., Danforth, C. W. 2012, ApJ, 752, 162; AGN composite spectra
(h) NIST http://physics.nist.gov/cgi-bin/ASD/lines1.pl
(i) Wiese, W. L.; Fuhr, J. R. (2009). "Accurate Atomic Transition Probabilities for Hydrogen, Helium, and Lithium". Journal of Physical and Chemical Reference Data. 38 (3): 565. Bibcode:2009JPCRD..38..565W. doi:10.1063/1.3077727.
(j) Estudio de estrellas masivas con espectros de alta resolución en los rangos ultravioleta lejano, ultravioleta y visible, Miriam Garcia PhD. 2005, ULL, Spain; massive star relevant lines

Air to vacuum conversions, when needed obtained from formulae at http://www.astro.uu.se/valdwiki/Air-to-vacuum%20conversion
Vacuum to air conversion from Eq. (1) in Morton 1991, ApJS 77, 119

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