2015A&A...576A..77S


Query : 2015A&A...576A..77S

2015A&A...576A..77S - Astronomy and Astrophysics, volume 576A, 77-77 (2015/4-1)

Molecfit: A general tool for telluric absorption correction. I. Method and application to ESO instruments.

SMETTE A., SANA H., NOLL S., HORST H., KAUSCH W., KIMESWENGER S., BARDEN M., SZYSZKA C., JONES A.M., GALLENNE A., VINTHER J., BALLESTER P. and TAYLOR J.

Abstract (from CDS):

The interaction of the light from astronomical objects with the constituents of the Earth's atmosphere leads to the formation of telluric absorption lines in ground-based collected spectra. Correcting for these lines, mostly affecting the red and infrared region of the spectrum, usually relies on observations of specific stars obtained close in time and airmass to the science targets, therefore using precious observing time. We present molecfit, a tool to correct for telluric absorption lines based on synthetic modelling of the Earth's atmospheric transmission. Molecfit is versatile and can be used with data obtained with various ground-based telescopes and instruments. Molecfit combines a publicly available radiative transfer code, a molecular line database, atmospheric profiles, and various kernels to model the instrument line spread function. The atmospheric profiles are created by merging a standard atmospheric profile representative of a given observatory's climate, of local meteorological data, and of dynamically retrieved altitude profiles for temperature, pressure, and humidity. We discuss the various ingredients of the method, its applicability, and its limitations. We also show examples of telluric line correction on spectra obtained with a suite of ESO Very Large Telescope (VLT) instruments. Compared to previous similar tools, molecfit takes the best results for temperature, pressure, and humidity in the atmosphere above the observatory into account. As a result, the standard deviation of the residuals after correction of unsaturated telluric lines is frequently better than 2% of the continuum. Molecfit is able to accurately model and correct for telluric lines over a broad range of wavelengths and spectral resolutions. The accuracy reached is comparable to or better than the typical accuracy achieved using a telluric standard star observation. The availability of such a general tool for telluric absorption correction may improve future observational and analysing strategies, as well as empower users of archival data.

Abstract Copyright:

Journal keyword(s): radiative transfer - atmospheric effects - instrumentation: spectrographs - methods: observational - methods: data analysis - techniques: spectroscopic

Simbad objects: 25

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Number of rows : 25
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 SCR J0103-5515 SB* 01 03 35.655120 -55 15 56.24316   16.99 15.40 14.96 12.09 M5.0 42 0
2 * alf For PM* 03 12 04.5298039833 -28 59 15.439152331 4.41 4.51 3.98 3.39 3.08 F6V 273 0
3 HD 269006 s*b 05 02 07.3942092168 -71 20 13.116800076 9.93 10.60 10.55 10.43 10.38 LBV 252 0
4 HD 34543 Pu* 05 13 25.1368579872 -65 14 09.981513204   8.30 8.37     B8V 36 0
5 * gam Gem SB* 06 37 42.71050 +16 23 57.4095 1.98 1.92 1.92 1.86 1.87 A1.5IV+ 510 1
6 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1865 0
7 * gam Cha V* 10 35 28.1055499388 -78 36 28.038741243 7.65 5.70 4.12 2.86 1.88 K4III 79 0
8 Cl* NGC 3603 MMM 117 * 11 15 07.6199053200 -61 15 30.252481236   15.27 14.17     O4V 9 0
9 V* DX Cha Ae* 12 00 05.0868602544 -78 11 34.565724312   6.81 6.60     A4V 344 0
10 HD 104327 PM* 12 00 48.1814978064 -37 28 45.251990832   8.72 8.28     F3V 23 0
11 [B2001b] IRS 1 Y*O 12 01 36.53040 -65 08 51.9180           ~ 153 0
12 BHR 71 MoC 12 01 37 -65 08.8           ~ 155 0
13 GRB 050730 gB 14 08 17.090 -03 46 18.90   20.32 17.68     ~ 314 0
14 GRB 080310 gB 14 40 13.89 -00 10 30.4           ~ 190 0
15 V* X TrA C* 15 14 19.1755012584 -70 04 46.113298104 15.88 9.19 5.81     C5,5 120 0
16 [GHE2001b] U69 XB* 17 40 40.867 -53 40 17.17   19.03   17.84   ~ 6 0
17 Cl* NGC 6397 PCBY 6 XB* 17 40 41.779 -53 40 14.42   19.88   18.45   ~ 6 0
18 NGC 6397 GlC 17 40 42.09 -53 40 27.6     5.17     ~ 1979 0
19 Cl* NGC 6397 SAW V18 EB* 17 40 43.47 -53 40 26.6   16.23 15.71     ~ 5 0
20 NAME Barnard's star BY* 17 57 48.4984700685 +04 41 36.113879676 12.497 11.24 9.511 8.298 6.741 M4V 815 2
21 2MASS J19444596-1451029 s*r 19 44 45.9748062120 -14 51 02.883440880   20.91 18.96 17.89   M/KI 6 0
22 CW Red 44 s*r 19 44 55.9214074320 -14 47 19.982762484   21.43 19.56 18.52   K5I 5 0
23 NGC 6822 G 19 44 56.199 -14 47 51.29   18 8.1     ~ 1563 0
24 [K67] V19 s*r 19 44 57.3122956968 -14 49 20.594970300   19.69 17.41 16.20   M1I 14 0
25 HD 187439 * 19 50 26.6386602672 -13 55 26.039188596   7.38 7.37     B5/7III 13 0

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