A dataset provided by the European Space Agency

Name VEGAMAIN
Title PHOT REOBSERVATION OF VEGA DISK STARS
URL

http://nida.esac.esa.int/nida-sl-tap/data?RETRIEVAL_TYPE=OBSERVATION&PRODUCT_LEVEL=ALL&obsno=527006230

DOI https://doi.org/10.5270/esa-4er6dzr
Author Stencel, R.E.
Description we request 7.7 hours of supplemental observing time in order to re-observe key early-release vega-disk sources that suffered from inadequate signal to noise observations during the early months of iso science operations. the 20 selected main sequence stars are part of our nasa guarranteed time program intended to determine the frequency of mid-infrared excesses among a volume-limited sample. we invested 18.8ksec in early release observations, but have not achieved useful s/n with p3 detector chopping observations. we request the opportunity to reobserve these objects using c100 chopping mode, (p22 and p37) which has proven successful as our current observing strategy with this program. ======================================================================== ==> in this proposal, more time is being requested for rstencel.vegadisk ========================================================================
Instrument PHT03 , PHT22 , PHT37 , PHT38 , PHT39
Temporal Coverage 1997-03-11T12:11:45Z/1997-05-03T10:21:34Z
Version 1.0
Mission Description The Infrared Space Observatory (ISO) was the worlds first true orbiting infrared observatory. Equipped with four highly-sophisticated and versatile scientific instruments, it was launched by Ariane in November 1995 and provided astronomers world-wide with a facility of unprecedented sensitivity and capabilities for a detailed exploration of the Universe at infrared wavelengths.
Creator Contact https://support.cosmos.esa.int/iso/
Date Published 1999-03-31T00:00:00Z
Keywords ISO, infrared, SWS, LWS, ISOCAM, ISOPHOT
Publisher And Registrant European Space Agency
Credit Guidelines European Space Agency, Stencel et al., 1999, 'PHOT REOBSERVATION OF VEGA DISK STARS', 1.0, European Space Agency, https://doi.org/10.5270/esa-4er6dzr