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Part 1: Document Description
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Citation |
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Title: |
Replication data for: Whole Galaxy |
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Identification Number: |
doi:10.7910/DVN/WH9OQR |
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Distributor: |
Harvard Dataverse |
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Date of Distribution: |
2011-10-18 |
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Version: |
3 |
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Bibliographic Citation: |
Dame, T. M.; Hartmann, Dap; Thaddeus, P., 2011, "Replication data for: Whole Galaxy", https://doi.org/10.7910/DVN/WH9OQR, Harvard Dataverse, V3 |
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Citation |
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Title: |
Replication data for: Whole Galaxy |
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Identification Number: |
doi:10.7910/DVN/WH9OQR |
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Authoring Entity: |
Dame, T. M. (Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138) |
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Hartmann, Dap (Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; Currently at Leiden Observatory, P.O. Box 9513, 2300 RA Leiden, The Netherlands) |
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Thaddeus, P. (Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138) |
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Distributor: |
Harvard Dataverse |
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Date of Deposit: |
2011-10-14 |
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Holdings Information: |
https://doi.org/10.7910/DVN/WH9OQR |
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Study Scope |
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Abstract: |
<p>Available data are raw, interpolated, and moment-masked versions of a large (1.3 GB) FITS cube containing the entire CO archive: all longitudes, all velocities (± 320 km/s), and ± 30° of latitude. While this cube can be very useful for large-scale Galactic studies, one should keep in mind that the component surveys vary somewhat in sensitivity, gridding, and velocity coverage. In numerous cases interpolation was required to force individual surveys onto the common <i>lbv</i> gr id. In general the <a href="http://dvn.theastrodata.org/dvn/dv/rtdc">individual CO surveys</a> will provide slightly higher data fidelity. </p> <p>The moment masked cube was not created directly from the raw cube, but rather is a composite of all the individual moment masked cubes. Each of these was "padded" with surrounding surveys before moment masking in order to avoid gaps in the composite cube between individual surveys owing to smoothing.</p> <p> The very large cubes of whole Galaxy are mainly empty, owing to the fact that the velocity spread of the emission is large only near the plane, and the latitude spread is large only near zero velocity. For these reasons, essentially all of the CO emission can be stored in two much smaller cubes, one restricted to a narrow latitude range ( ± 5° COGAL_deep.fits) and another restricted to a fairly narrow velocity range (± 35 km/s; COGAL_local.fits). The former is most useful for large-scale Galactic studies while the latter is best suited for studies of the solar neighborhood. </p> |
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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 href="http://adsabs.harvard.edu/abs/2001ApJ...547..792D">The Astrophysical Journal, Volume 547, Issue 2, pp. 792-813.</a> |
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Identification Number: |
2001ApJ...547..792D |
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Bibliographic Citation: |
<a href="http://adsabs.harvard.edu/abs/2001ApJ...547..792D">The Astrophysical Journal, Volume 547, Issue 2, pp. 792-813.</a> |
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Label: |
COGAL_all_interp.fits.gz |
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Text: |
Whole Galaxy FITS cube (all l, b, v), interpolated. In each spectrum, <= 2 missing channels are filled by linear interpolation. In each spatial plane, single missing pixels are filled by linear interpolation, first in l direction, then b. |
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Notes: |
application/x-gzip |
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Label: |
COGAL_all_mom.fits.gz |
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Text: |
Whole Galaxy FITS cube (all l, b, v), moment masked |
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Notes: |
application/x-gzip |
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Label: |
COGAL_all_raw.fits.gz |
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Text: |
Whole Galaxy FITS cube (all l, b, v), raw |
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Notes: |
application/x-gzip |
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Label: |
COGAL_all_raw.txt |
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Text: |
FITS header for whole Galaxy cube (all l, b, v) |
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Notes: |
text/plain; charset=US-ASCII |
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Label: |
COGAL_deep_interp.fits.gz |
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Text: |
Whole Galaxy "Deep" FITS cube (restricted to ± 5° in b), interpolated. In each spectrum, <= 2 missing channels are filled by linear interpolation. In each spatial plane, single missing pixels are filled by linear interpolation, first in l direction, then b. |
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Notes: |
application/x-gzip |
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Label: |
COGAL_deep_mom.fits.gz |
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Text: |
Whole Galaxy "Deep" FITS cube (restricted to ± 5° in b), moment masked |
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Notes: |
application/x-gzip |
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Label: |
COGAL_deep_raw.fits.gz |
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Text: |
Whole Galaxy "Deep" FITS cube (restricted to ± 5° in b), raw |
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Notes: |
application/x-gzip |
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Label: |
COGAL_deep_raw.txt |
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Text: |
FITS header for whole Galaxy "Deep" cube (restricted to ± 5° in b) |
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Notes: |
text/plain; charset=US-ASCII |
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Label: |
COGAL_local_interp.fits.gz |
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Text: |
Whole Galaxy "Local" FITS cube (restricted to ± 35 km/s), interpolated. In each spectrum, <= 2 missing channels are filled by linear interpolation. In each spatial plane, single missing pixels are filled by linear interpolation, first in l direction, then b. |
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Notes: |
application/x-gzip |
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Label: |
COGAL_local_mom.fits.gz |
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Text: |
Whole Galaxy "Local" FITS cube (restricted to ± 35 km/s), moment masked |
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Notes: |
application/x-gzip |
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Label: |
COGAL_local_raw.fits.gz |
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Text: |
Whole Galaxy "Local" FITS cube (restricted to ± 35 km/s) , raw |
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Notes: |
application/x-gzip |
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Label: |
COGAL_local_raw.txt |
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Text: |
FITS header for whole Galaxy "Local" cube (restricted to ± 35 km/s) |
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Notes: |
text/plain; charset=US-ASCII |