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Part 1: Document Description
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Citation |
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Title: |
Replication data for: The disk-bearing young star IM Lupi. X-ray properties and limits on accretion |
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Identification Number: |
doi:10.7910/DVN/TO6U8U |
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Distributor: |
Harvard Dataverse |
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Date of Distribution: |
2013-05-16 |
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Version: |
1 |
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Bibliographic Citation: |
Günther, H. M; Matt, S. P.; Schmitt, J. H. M. M.; Güdel, M.; Li, Z.-Y.; Burton, D. M., 2013, "Replication data for: The disk-bearing young star IM Lupi. X-ray properties and limits on accretion", https://doi.org/10.7910/DVN/TO6U8U, Harvard Dataverse, V1 |
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Citation |
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Title: |
Replication data for: The disk-bearing young star IM Lupi. X-ray properties and limits on accretion |
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Identification Number: |
doi:10.7910/DVN/TO6U8U |
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Authoring Entity: |
Günther, H. M (Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany ; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA) |
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Matt, S. P. (NASA Ames Research Center, Moffett Field, CA 94035, USA) |
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Schmitt, J. H. M. M. (Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany) |
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Güdel, M. (Institute of Astronomy, ETH Zürich, 8093 Zürich, Switzerland; Department of Astronomy, University of Vienna, Türkenschanzstr. 17, 1180 Vienna, Austria) |
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Li, Z.-Y. (Department of Astronomy, University of Virginia, PO Box 400325, Charlottesville, VA 22904, USA) |
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Burton, D. M. (Department of Astronomy, University of Virginia, PO Box 400325, Charlottesville, VA 22904, USA), AF(University of Southern Queensland, Toowoomba Qld 4350, Australia) |
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Grant Number: |
50OR0105 |
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Distributor: |
Harvard Dataverse |
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Date of Deposit: |
2013-05-16 |
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Holdings Information: |
https://doi.org/10.7910/DVN/TO6U8U |
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Study Scope |
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Abstract: |
This archive contains the AAO data used in the referenced publication. The Chandra and ESO/HARPS data can be downloaded from the respective institutional archives. Some information on the data format is below, see the original publication for details. The reduced spectra have not been spliced together and the continuum fitting is not perfect in the blue orders. In addition, I think the extraction of the first order (in the blue) is not the best and should probably be treated cautiously. The spectra have been shifted to match the telluric lines in each spectrum and some pixels have been removed (due to poor fitting) which is why each spectrum has a different number of datapoints. The reduced spectra are just ASCII files with 3 columns, the first is wavelength (in nm), the second is the normalised intensity, and the 3rd is a measure of the error in the intensity at each pixel. The first 2 rows of the file contain header information. Dates of observation 4 exp.; 30 min each two consequtive on each day UTC MJD 2009-05-05T12:38:14.5 5.495652652204E+04 2009-05-05T13:08:31.5 5.495654755213E+04 2009-05-06T11:49:32.5 5.495749271413E+04 2009-05-06T12:19:49.5 5.495751374479E+04 |
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Methodology and Processing |
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Sources Statement |
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Data Access |
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Notes: |
<a href="http://creativecommons.org/publicdomain/zero/1.0">CC0 1.0</a> |
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Other Study Description Materials |
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Related Publications |
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Citation |
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Title: |
A&A, 519, A97 (2010) |
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Identification Number: |
10.1051/0004-6361/201014386 |
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Bibliographic Citation: |
A&A, 519, A97 (2010) |
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Label: |
IMLup_05may_35_dopcor.dat |
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Text: |
AAO spectrum, see study description for the data reduction |
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Notes: |
text/plain; charset=US-ASCII |
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Label: |
IMLup_05may_36_dopcor.dat |
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Text: |
AAO spectrum, see study description for the data reduction |
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Notes: |
text/plain; charset=US-ASCII |
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Label: |
IMLup_06may_36_dopcor.dat |
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Text: |
AAO spectrum, see study description for the data reduction |
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Notes: |
text/plain; charset=US-ASCII |
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Label: |
IMLup_06may_37_dopcor.dat |
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Text: |
AAO spectrum, see study description for the data reduction |
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Notes: |
text/plain; charset=US-ASCII |