Submillimeter follow up_of_wise_selected_hyperluminous_galaxies
Submillimeter Data for SINGS George J. Bendo & Robert D. Joseph (A ''George's Adventures in Learning...
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Transcript of Submillimeter Data for SINGS George J. Bendo & Robert D. Joseph (A ''George's Adventures in Learning...
Submillimeter Data for SINGS
George J. Bendo & Robert D. Joseph
(A ''George's Adventures in Learning OpenOffice'' Presentation)
Outline
● Overview of JCMT and SCUBA
● Basic data processing
● Current archival data
● Future observations
James Clerck Maxwell Telescope
● 15 m submillimeter telescope
● Located on Mauna Kea (elevation 4,090 m)
● Began operating in 1987
● Operated by Joint Astronomy Center
● UK controls most observing time; Canada, Netherlands, Hawaii also get shares
● Instruments include bolometer array (SCUBA) and heterodyne receivers
SCUBA (Submillimeter Common-User Bolometer Array)
● Two sets of bolometers that can observe the same field simultaneously
– 91 element short wavelength (450 m) array
– 37 element long wavelength (850 m) array● 3 longer wavelength (1.1, 1.35, 2.0 mm) bolometers flank the long
wavelength array but are rarely used
● Arrays can be used in three basic observing modes
– Stare photometry
– Jiggle map
– Scan map
SCUBA Processing Software
Because the data comes in terms of bolometer signal measurements over time, special software is needed to process the data into intensity maps .
The JAC has created the SURF package, which works with other Starlink packages and data in the NDF (N-dimensional Data File) format.
Basic SCUBA Processing(Steps for all observing modes)
● reduce_switch Split data into individual bolometer signals
● flatfield Flatfields the data
● extinction Corrects the data for atmospheric extinction; also splits the data into short and long wavelength components
● change_quality Remove ''bad'' bolometers (i.e. bolometers producing noisy data)
● despike2, scuclip Remove data spikes
Jiggle Map / Stare PhotometryData Processing
● remsky Remove background as well as systematic variations across image from sky noise
● rebin Combines multiple data files and rebins the data in RA and declination
Scan Map Data Processing
● scan_rlb Remove variations in offset from bolometer to bolometer
● calcsky, remsky Remove background as well as systematic variations across image from sky
noise
● rebin Rebins the data in RA and declination for each individual scan
● remdbm Combines all individual scans into a final image
Calibration
● Planets (especially Uranus and Mars) favored
● Secondary calibrators (mostly planetary nebulae) also used
● JCMT documentation treats source calibration as though sources are similar to point sources but these instructions will be disregarded when calibrating SINGS data
● Calibrator counts will be measured in 2' aperture to create calibration factor to apply to maps after processing
Final Maps
● Images will be in fits format
● Data will be calibrated in Jy
● Beam sizes are approximately ~8” at 450m and ~15” at 850m
● Image scales will be 1” / pixel (but scale can be adjusted)
● Image artifacts may be present
– Hexagonal image edges
– Hot pixels (particularly around edges of pointings
– Holes in images (where bolometers masked out)
– Grainy sky-noise
– Large scale background fluctuations in scan maps
SINGS data in SCUBA archive
24 SINGS galaxies found in SCUBA archives
– 8 galaxies are non-detections
– 8 galaxies are detections but contain no significant signal outside the nucleus
– 8 galaxies contain detections of extended structure (although these structures are sometimes small)
Planned JCMT Observations
● Proposed observations through R. D. Joseph at University of Hawaii
● 9 shifts awarded as part of flexible observing
– Proposal ranked 8 out of 16
– Requested conditions for observing 850 m (450 m possible but unlikely)
– 5 shifts given high priority (observations likely)
– 4 shifts given low priority (observations made only if weather is good)
● Estimate that at least 12 - 13 galaxies can be observed
● Data will consist of jiggle maps covering central 2.6' x 2.3'
Future Submillimeter Observations
● JCMT
– Most sensitive telescope at both 450 & 850 m
– Best at resolving and mapping moderately extended objects
– Multiple wavelength observations possible
– Difficult to apply directly; must apply through collaborators at institutions with access to telescope (but we will probably have future access through Hawaii)
Future Submillimeter Observations (continued)
● HHST (Heinrich Hertz Submillimeter Telescope)
– Scan mapping capabilities at 850 m (but mapping mode is inefficient)
– Easily accessible to Steward Observatory staff
– Lower sensitivity (~5x)● CSO (Caltech Submillimeter Observatory)
– Scan and stare mapping modes at 350, 450, & 850 m
– Easily accessible to Caltech staff
– Optomized for 350 m, which is exceedingly difficult; longer wavelength observations inferior to JCMT