CASA, the Common Astronomy Software Applications for Radio Astronomy

TEAM, THE CASA; Bean, Ben; Bhatnagar, S.; Castro, S.; Meyer, Jennifer Donovan; Emonts, Bjorn; García, Enrique Rivera; Garwood, Robert; Golap, K.; Villalba, Justo Gonzalez; Harris, Pamela E.; Hayashi, Yu-ichi; Hoskins, Josh; Hsieh, Ming-Yu; Jagannathan, P.; Kawasaki, Wataru; Keimpema, A.; Kettenis, Mark; López, J. Castro; Marvil, J.; Masters, J.; McNichols, Andrew; Mehringer, David M.; Miel, Renaud; Moellenbrock, G.; Montesino, Federico; Nakazato, Takeshi; Ott, J.; Petry, D.; Pokorný, Martin; Raba, Ryan; Rau, Urvashi; Schiebel, Darrell; Schweighart, Neal; Sekhar, Srikrishna; Shimada, Kaoru; Small, Des; Steeb, Jan-Willem; Sugimoto, Kunihisa; Suoranta, Ville; Tsutsumi, Takahiro; Bemmel, I. M. van; Verkouter, Marjolein; Wells, Akeem; Xiong, Wei; Szomoru, Arpad; Griffith, Morgan; Glendenning, Brian; Kern, J.

doi:10.1088/1538-3873/ac9642

Cited by 327 publications

(55 citation statements)

References 88 publications

(86 reference statements)

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“…) package version 5.6.1 (McMullin et al 2007;CASA Team et al 2022), while the 12 m Array data were pipeline-calibrated with the same version of . This included all the standard calibration steps applied to the phases and the amplitudes of the data.…”

Section: Alma Observations and Data Processingmentioning

confidence: 99%

The Bright Extragalactic ALMA Redshift Survey (BEARS) II: Millimetre photometry of gravitational lens candidates

Bendo¹,

Urquhart²,

S.³

et al. 2023

Preprint

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Section: Alma Observations and Data Processingmentioning

confidence: 99%

The Bright Extragalactic ALMA Redshift Survey (BEARS) II: Millimetre photometry of gravitational lens candidates

Bendo¹,

Urquhart²,

S.³

et al. 2023

Preprint

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“…To investigate the origin of the feature, we simulate the observation with a similar setup: hour angle, sky position, antenna configuration, and realistic atomospheric noise, but without emission in the sky, using SIMALMA in CASA. 20 (The actual data are taken with ∼2 h observation, with 1 h of integration on a source intermittently separated by calibrator observations and other overheads. In comparison, the simulated observation is a continuous 1 h of integration on the source.)…”

Section: Discussionmentioning

confidence: 99%

Estimating the statistical uncertainty due to spatially correlated noise in interferometric images

Tsukui

Iguchi

Mitsuhashi

et al. 2023

J. Astron. Telesc. Instrum. Syst.

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Interferometers (e.g., ALMA and NOEMA) allow us to obtain the detailed brightness distribution of astronomical sources in three dimensions (R.A., Dec., and frequency). However, the spatial correlation of the noise makes it difficult to evaluate the statistical uncertainty of the measured quantities and the statistical significance of the results obtained. The noise correlation properties in the interferometric image are fully characterized and easily measured by the noise autocorrelation function (ACF). We present the method for (1) estimating the statistical uncertainty due to the correlated noise in the spatially integrated flux and spectra directly, (2) simulating the correlated noise to perform a Monte Carlo simulation in image analyses, and (3) constructing the covariance matrix and chi-square χ 2 distribution to be used when fitting a model to an image with spatially correlated noise, based on the measured noise ACF. We demonstrate example applications to scientific data showing that ignoring noise correlation can lead to significant underestimation of statistical uncertainty of the results and false detections/ interpretations.

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“…We use Common Astronomy Software Applications (CASA, CASA Team et al 2022) to reduce the data and perform imaging. A spectral cube is created using tclean task with natural weighting and a 100 km s −1 channel width.…”

Section: Sample and Data Analysismentioning

confidence: 99%

Characterizing CO Emitters in SSA22-AzTEC26 Field

Huang¹,

Umehata²,

Kawabe³

et al. 2023

Preprint

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We report the physical characterization of four CO emitters detected near the bright submillimeter galaxy (SMG) SSA22-AzTEC26. We analyze the data from ALMA band 3, 4, and 7 observations of the SSA22-AzTEC26 field. In addition to the targeted SMG, we detect four line emitters with a signalto-noise ratio > 5.2 in the cube smoothed with 300 km s −1 FWHM Gaussian filter. All four sources have near-infrared (NIR) counterparts within 1 arcsec. We perform ultraviolet to far-infrared spectral energy distribution (SED) modeling to derive the photometric redshift and physical properties. Based on photometric redshifts, we reveal that two of them are CO(2-1) at redshifts of 1.113 and 1.146, and one is CO(3-2) at z = 2.124. The three sources are massive galaxies with a stellar mass 10 10.5 M , but have different levels of star formation. Two lie within the scatter of the main sequence (MS) of star-forming galaxies at z ∼ 1 − 2, and the most massive galaxy lies significantly below the MS. However, all three sources have a gas fraction within the scatter of the MS scaling relation. This shows that a blind CO line search can detect massive galaxies with low specific star formation rates that still host large gas reservoirs and complements targeted surveys, suggesting later gas acquisition and the need for other mechanisms in addition to gas consumption to suppress the star formation.

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CASA, the Common Astronomy Software Applications for Radio Astronomy

Cited by 327 publications

References 88 publications

The Bright Extragalactic ALMA Redshift Survey (BEARS) II: Millimetre photometry of gravitational lens candidates

The Bright Extragalactic ALMA Redshift Survey (BEARS) II: Millimetre photometry of gravitational lens candidates

Estimating the statistical uncertainty due to spatially correlated noise in interferometric images

Characterizing CO Emitters in SSA22-AzTEC26 Field

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