First observations with SuperCam and future plans

Kloosterman, Jenna; Cottam, T.; Swift, B.; Lesser, David; Schickling, Paul; Groppi, Christopher; Borden, Michael; Towner, A. P.; Schmidt, Per; Kulesa, Craig; d’Aubigny, C. Drouet; Walker, Christopher K.; Golish, D. R.; Weinreb, S.; Jones, Glenn; Mani, H. S.; Kooi, J.; Lichtenberger, A. W.; Puetz, P.; Narayanan, Gopal

doi:10.1117/12.925088

Cited by 10 publications

(5 citation statements)

References 1 publication

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“…For a description of the instrument, see Kloosterman et al (2012). In brief, the receiver consists of a square array of 8×8 superconductor-insulator-superconductor mixers, each with a cooled first-stage IF amplifier.…”

Section: J=3−2 Linementioning

confidence: 99%

THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. V. THE SH2-235 CLOUD IN CO J = 2 − 1, ¹³CO J = 2 − 1, AND CO J = 3 − 2

Bieging

Patel

Peters

et al. 2016

ApJS

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We present the results of a program to map the Sh2-235 molecular cloud complex in the CO and 13 COJ=2−1 transitions using the Heinrich Hertz Submillimeter Telescope. The map resolution is 38″ (FWHM), with an rms noise of 0.12 K brightness temperature, for a velocity resolution of 0.34 km s −1. With the same telescope, we also mapped the CO J=3−2 line at a frequency of 345 GHz, using a 64 beam focal plane array of heterodyne mixers, achieving a typical rms noise of 0.5 K brightness temperature with a velocity resolution of 0.23 km s −1. The three spectral line data cubes are available for download. Much of the cloud appears to be slightly sub-thermally excited in the J=3 level, except for in the vicinity of the warmest and highest column density areas, which are currently forming stars. Using the CO and 13 COJ=2−1 lines, we employ an LTE model to derive the gas column density over the entire mapped region. Examining a 125 pc 2 region centered on the most active star formation in the vicinity of Sh2-235, we find that the young stellar object surface density scales as approximately the 1.6-power of the gas column density. The area distribution function of the gas is a steeply declining exponential function of gas column density.Comparison of the morphology of ionized and molecular gas suggests that the cloud is being substantially disrupted by expansion of the H II regions, which may be triggering current star formation.

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Section: J=3−2 Linementioning

confidence: 99%

THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. V. THE SH2-235 CLOUD IN CO J = 2 − 1, ¹³CO J = 2 − 1, AND CO J = 3 − 2

Bieging

Patel

Peters

et al. 2016

ApJS

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“…The implementation using ORAC-DR can only be used with raw data written using the JCMT data model (Appendix A). Some work has been done on software to import data from Supercam (Kloosterman et al 2012) and NANTEN2 SMART (Graf et al 2008) into the JCMT format and tests are ongoing. We hope that this work will influence the data acquisition and data processing plans for other observatories building large focal plane arrays.…”

Section: Resultsmentioning

confidence: 99%

“…As heterodyne receivers have progressed from single-detector instruments (Padman et al 1992;Davies et al 1992;Cunningham et al 1992) to small focal-plane arrays (Graf et al 2003;Schuster et al 2004) to 16-element arrays such as HARP at JCMT (Buckle et al 2009), and beyond (Kloosterman et al 2012;Hurtado et al 2014), and correlators have improved such that we can easily obtain spectra at 10 Hz with 8192 channels, data rates have increased substantially such that it is now common-place to take a short observation resulting in thousands of spectra. This is only going to become more challenging with the advent of instruments with 64,000 channels and dual-waveband arrays each of which consist of 128 detectors, such as the CHAI instrument proposed for CCAT or KAPPa successors (Wheeler et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Automated reduction of sub-millimetre single-dish heterodyne data from the James Clerk Maxwell Telescope using orac-dr

Jenness

Currie

Tilanus

et al. 2015

Mon. Not. R. Astron. Soc.

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With the advent of modern multi-detector heterodyne instruments that can result in observations generating thousands of spectra per minute it is no longer feasible to reduce these data as individual spectra. We describe the automated data reduction procedure used to generate baselined data cubes from heterodyne data obtained at the James Clerk Maxwell Telescope. The system can automatically detect baseline regions in spectra and automatically determine regridding parameters, all without input from a user. Additionally it can detect and remove spectra suffering from transient interference effects or anomalous baselines. The pipeline is written as a set of recipes using the ORAC-DR pipeline environment with the algorithmic code using Starlink software packages and infrastructure. The algorithms presented here can be applied to other heterodyne array instruments and have been applied to data from historical JCMT heterodyne instrumentation.

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“…For instance, it was used to map a 2.7 square degree area of the Orion molecular cloud complex (Stanke et al 2022). For more technical details of the array receiver, we refer to Groppi et al (2010) and Kloosterman et al (2012).…”

Section: Co(3-2) Observationsmentioning

confidence: 99%

SuperCAM CO(3–2) APEX survey at a 6 pc resolution in the Small Magellanic Clouds

Saldaño,

Rubio,

Bolatto

et al. 2024

A&A

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The Small Magellanic Cloud (SMC) is an ideal laboratory for studying the properties of star-forming regions thanks to its low metallicity, which has an impact on the molecular gas abundance. However, a small number of molecular gas surveys of the entire galaxy have been carried out in the last few years, limiting the measurements of interstellar medium (ISM) properties in a homogeneous manner. We present the CO($3-2$) APEX survey at a $6$ pc resolution of the bar of the SMC, observed with the SuperCAM receiver attached to the APEX telescope. This high-resolution survey has allowed us to study certain properties of the ISM and to identify CO clouds in the innermost parts of the H$_2$ envelopes. We black adopted the CO analysis in the SMC bar comparing the CO($3-2$) survey with that of the CO($2-1$) of a similar resolution. We studied the CO($3-2$)-to-CO($2-1$) ratio ($R_ $), which is very sensitive to the environment properties (e.g., star-forming regions). We analyzed the correlation of this ratio with observational quantities that trace the star formation such as the local CO emission, the Spitzer color $ $, and the total IR surface brightness measured from the Spitzer and Herschel bands. For the identification of the CO($3-2$) clouds, we used the CPROPS algorithm, which allowed us to measure the physical properties of the clouds. We analyzed the scaling relationships of such physical properties. black We obtained $R_ 0.02$ for the SW bar and a slightly higher ratio 0.1,$ for N66 in the SMC. We found that $R_ $ varies from region to region, depending on the star formation activity. In regions dominated by HII and photo-dissociated regions (e.g., N22, N66) $R_ $ tends to be higher than the median values. Meanwhile, lower values were found toward quiescent clouds. We also found that $R_ black is correlated with the IR color $ $ and the total IR surface brightness. This finding indicates that $R_ $ increases with environmental properties, such as the dust temperature, total gas density, and radiation field. We identified $225$ molecular clouds with sizes of $R > 1.5$ pc and signal-to-noise ratios (S/N) of $> 3$ black of which only $17$ black are well resolved CO($3-2$) clouds black with S/N $ 5$. These $17$ clouds follow consistent scaling relationships to the inner Milky Way clouds but with some departures. For instance, CO($3-2$) tends to be less turbulent and less luminous than the inner Milky Way clouds of similar sizes. Finally, we estimated a median virial-based CO($3-2$)-to-H$_2$ conversion factor of for the total sample.

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First observations with SuperCam and future plans

Cited by 10 publications

References 1 publication

THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. V. THE SH2-235 CLOUD IN CO J = 2 − 1, ¹³CO J = 2 − 1, AND CO J = 3 − 2

THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. V. THE SH2-235 CLOUD IN CO J = 2 − 1, ¹³CO J = 2 − 1, AND CO J = 3 − 2

Automated reduction of sub-millimetre single-dish heterodyne data from the James Clerk Maxwell Telescope using orac-dr

SuperCAM CO(3–2) APEX survey at a 6 pc resolution in the Small Magellanic Clouds

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First observations with SuperCam and future plans

Cited by 10 publications

References 1 publication

THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. V. THE SH2-235 CLOUD IN CO J = 2 − 1, 13CO J = 2 − 1, AND CO J = 3 − 2

THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. V. THE SH2-235 CLOUD IN CO J = 2 − 1, 13CO J = 2 − 1, AND CO J = 3 − 2

Automated reduction of sub-millimetre single-dish heterodyne data from the James Clerk Maxwell Telescope using orac-dr

SuperCAM CO(3–2) APEX survey at a 6 pc resolution in the Small Magellanic Clouds

Contact Info

Product

Resources

About

THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. V. THE SH2-235 CLOUD IN CO J = 2 − 1, ¹³CO J = 2 − 1, AND CO J = 3 − 2

THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. V. THE SH2-235 CLOUD IN CO J = 2 − 1, ¹³CO J = 2 − 1, AND CO J = 3 − 2