1. spectrophotometrypaper.pdf Spectrophotometry: Revised Standards and Techniques Authors: Bessell, Michael S. Affiliation: Research School of Astronomy and Astrophysics, Institute of Advanced Studies, The Australian National University, Private Bag, Weston Creek P.O., ACT 2611, Australia; bessell@mso.anu.edu.au Journal: PASP 111, 1426-1433 1999 cuarti.arc line list for CuAr and NeAr lamp (Ti contaminants) arlines.300b identification for 300B grating arlines.316r identification of DBS red 316R grating arlines.600b identification of DBS blue 600l/mm grating arlines.redcuar identification of DBS red 1200l/mm grating arlines.rednearw identification of DBS red 1200l/mm grating blue.gif.tar finding charts for blue stars faint.gif.tar finding charts for standard stars The extinction tables are the continous extinctions not including H2O and O2 and needed in this form when you take out the molecules by smooth spectrum star division. extin.tab Mean Extinction Coefficients for Palomar Mountain Hayes & Latham 1975, Ap.J. 197, p597 extinaao.tab Mean Extinction Coefficients for AAO 3000 - 11000 50A steps extrapolated from extinsso.tab extinsso.tab A A O E X T . T A B Based on Hayes and Latham. The following are Hamuy standards corrected for the presence of water and O2. cd32a.tab f56a.tab hr718.tab l2415.tab l6248a.tab eg131a.tab h600.tab hr718a.tab l2415a.tab l7379.tab eg21.tab h600a.tab hr7596.tab l3218.tab l7987.tab eg21a.tab hr1544.tab hr7596a.tab l3218a.tab l7987a.tab eg274.tab hr1544a.tab hr7950.tab l377.tab l9239.tab eg274a.tab hr3454.tab hr7950a.tab l377a.tab l9239a.tab ex274.tab hr3454a.tab hr8634.tab l3864.tab l9491.tab extin.tab hr4468.tab hr8634a.tab l3864a.tab l9491a.tab extinaao.tab hr4468a.tab hr9087.tab l4364.tab one.tab extinsso.tab hr4963.tab hr9087a.tab l4364a.tab f110.tab hr4963a.tab l1020.tab l4816.tab f110a.tab hr5501.tab l1020a.tab l4816a.tab f56.tab hr5501a.tab l1788.tab l6248.tab VMa2_model.txt and VMa2_modela.txt are VMa2 model fits by Wolff, Koester and Liebert 2002. vma2.tab and vma2a.tab is Oke MCS spectrum of VMa2 (bumps redward of CaK are not real). l745.bbfit is blackbody fit to the Oke continuum of L745-46a NOTE: l745-46anew.tab, hd26169.tab and ltt4364new.tab were determined by Bessell in Jan 2009 using the Gregg-Heap spectra (below)as standards. ** spectro.coord is the list of stars in PASP 111. ** ************************************************************************* added in 2008/2009 BETTER STANDARDS are the following list gregg_stds.coord that contains some brighter subdwarf stars with STIS spectra. These STIS spectra have be rereduced by Heap and Lindler see http://archive.stsci.edu/prepds/stisngsl/index.html The stars labelled Bessell or Hamuy are some kept from the earlier standard list. %star ra2000 dec2000 V B-V m-M Mv d [M/H] "vma2" 00 49 10 +05 23 24 ! 12.38 0.550 DG Bessell "hd8724" 1 26 17.6 17 07 35.1 ! 8.30 0.960 7.59 0.71 -1.8 "hd9051" 1 28 46.5 -24 20 25.4 ! 8.93 0.820 11.18 -1.6 "hd16031" 2 34 11.0 -12 23 03.5 ! 9.77 0.437 5.31 4.46 d -1.8 "hd19445" 3 08 25.6 26 19 51.4 ! 8.04 0.486 2.94 5.10 d -2.0 "HD26169" 04 00 52.5 -75 36 11.4 ! 8.9 near Magellanic Clouds Bessell "hd26297" 4 09 03.4 -15 53 27.1 ! 7.46 1.088 9.46 -2.00 -1.7 "hd29574" 4 38 55.7 -13 20 48.1 ! 8.33 1.304 10.90 -2.57 -1.9 "hd36702" 5 31 52.2 -38 33 24.0 ! 8.33 1.148 10.84 -2.51 -2.0 "hd44007" 6 18 48.5 -14 50 43.4 ! 8.05 0.829 6.43 1.62 d -1.7 "hd45282" 6 26 40.8 03 25 29.8 ! 8.00 0.703 5.67 2.33 d -1.5 "hd55496" 7 12 11.4 -22 59 00.6 ! 8.37 0.955 8.06 0.31 -1.5 "l745-46a" 07 40 21 -17 24 54 ! 13.03 0.245 DF Bessell "bd-12_2669" 8 46 39.6 -13 21 25.4 ! 10.24 0.311 6.20 4.04 d -1.5 "hd83212" 9 36 20.0 -20 53 14.8 ! 8.33 1.015 8.54 -0.21 -1.5 "ltt4364" 11 45 43 -64 50 24 ! 11.51 0.190 DC(C2) Bessell "g13-35" 12 25 35.0 01 17 02.3 ! 9.66 0.445 4.80 4.86 d -1.8 "hd118055" 13 34 39.9 -16 19 22.7 ! 8.86 1.268 10.90 -2.04 -1.8 "hd122956" 14 05 13.0 -14 51 25.5 ! 7.22 0.939 7.41 -0.19 -1.6 "hd128279" 14 36 48.5 -29 06 46.7 ! 8.02 0.640 6.12 1.90 -2.1 "g20-15" 17 47 28.0 -08 46 47.7 ! 10.60 0.605 4.93 5.67 d -1.8 "hd161770" 17 47 46.1 -09 36 18.5 ! 9.68 0.672 4.87 4.81 d -2.1 "hd165195" 18 04 40.1 03 46 44.7 ! 7.31 1.232 8.29 -0.98 -2.2 "eg131" 19 20 35 -07 40 06 ! 12.28 0.04 DC Bessell "hd184266" 19 34 15.4 -16 19 00.2 ! 7.59 0.548 7.42 0.17 d -1.8 "hd187111" 19 48 39.6 -12 07 19.7 ! 7.71 1.171 8.51 -0.80 -1.7 "g24-3" 20 05 44.3 04 02 52.8 ! 10.46 0.510 6.37 4.09 d -1.7 "cd-30_18140"20 44 06.3 -30 00 07.6 ! 9.94 0.428 5.68 4.26 d -2.2 "hd204543" 21 29 28.2 -03 30 55.4 ! 8.28 0.888 -1.8 "bd+17_4708" 22 11 31.4 18 05 34.2 ! 9.46 0.459 5.37 4.09 d -1.7 "g29-23" 23 19 40.5 03 22 16.7 ! 10.21 0.456 7.43 2.78 d -1.8 "ltt9491" 23 19 35.0 -17 05 24.0 ! 14.10 0.029 DB3 HST Hamuy "f110" 23 19 58 -05 09 54 ! 11.85 -0.304 sdO HST Hamuy These new spectral standards are very precise STIS stars observed by Michael Gregg and rereduced by Heap and Lindler. Interim reduced spectra are made available by Sarah Heap and Don Lindler. See http://archive.stsci.edu/prepds/stisngsl/index.html ** EG131 is a near blackbody of about 11800K. It only has a very weak Halpha line about 5% deep. L745-46a has Ca HK lines and a very weak NaD line 2% deep and an Halpha line about 5% deep. These lines can be edited out before smoothing and dividing through all extracted spectra to remove the instrumental response. LTT4364 is also a near blackbody. It has weak shallow C2-Swan bands. F110 is a sdO star with weak He and H lines and much UV flux. ********** l745-46anew.tab, hd26169.tab and ltt4364new.tab are determined by Bessell in Jan 2009 using the Gregg-Heap spectra as standards. **************** 2) bessell2007BJ.pdf is a 2007 PASP 119 paper on measuring Balmer Jumps in stars. ** 3) bcp98.pdf is 1998 paper on synthetic photometry from the Kurucz-Castelli and Plez spectra. Appendix details much useful information on colours magnitudes and bolometric corrections. Note that in Table A2 the labels zp(Flambda) and zp(Fnu) should be reversed. The fourth row is zp(Fnu). ** 4) araapaper_bessell.pdf is the ARAA paper on Standard Systems. -------------------------------------------------------------------- figcommands.com are a list of instructions for wavelength calibrating, extinction correction and relative-absolute flux correction of extracted spectra using FIGARO. Normally all spectra are divided through by the normalised extracted spectrum of a "smooth spectrum" star, such as EG131 or L745-46A or L4364 after removing the Halpha (eg131, l745-46a), CaHK (l745-47a) and C2 bands (l4364) first. These should be observed at reasonably low airmass (1.0-1.2). It is a good idea to subtract 1.0 from all airmasses when correcting for extinction. That way the extinction corrections made are smaller and the extinction-corrected divided-by-the-smooth-spectrum-star resultant calibration curve is reasonably flat and well fitted by a polynomial or spline. CORRECTING FOR ADDITIONAL TELLURIC in the red the division by a smooth spectrum star in the red does remove telluric lines to the first order. To remove the remaining telluric lines you need to normalize (flatten) the spectrum of the smooth template then raise it to different powers and test divide by them until you find one that makes the bands vanish. Wade and Horn suggest that scaling by (secz)^0.6 corrects the O2 and H2O bands.