Searching for codes credited to 'Blanc, Guillermo A.'
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[ascl:2105.020]
PAP: PHANGS-ALMA pipeline
Leroy, Adam K.;
Hughes, Annie;
Liu, Daizhong;
Pety, Jerome;
Rosolowsky, Erik;
Saito, Toshiki;
Schinnerer, Eva;
Schruba, Andreas;
Usero, Antonio;
Faesi, Christopher M.;
Herrera, Cinthya N.;
Chevance, Melanie;
Hygate, Alexander P. S.;
Kepley, Amanda A.;
Koch, Eric W.;
Querejeta, Miguel;
Sliwa, Kazimierz;
Will, David;
Wilson, Christine D.;
Anand, Gagandeep S. Barnes, Ashley;
Belfiore, Francesco;
Beslic, Ivana;
Bigiel, Frank;
Blanc, Guillermo A.;
Bolatto, Alberto D.;
Boquien, Mederic;
Cao, Yixian;
Chandar, Rupali;
Chastenet, Jeremy;
Chiang, I-Da;
Congiu, Enrico;
Dale, Daniel A.;
Deger, Sinan;
den Brok, Jakob S.;
Eibensteiner, Cosima;
Emsellem, Eric;
Garcıa-Rodrıguez, Axel;
Glover, Simon C. O.;
Grasha, Kathryn;
Groves, Brent;
Henshaw, Jonathan D.;
Jimenez Donaire, Maria J.;
Kim, Jenny J.;
Klessen, Ralf S.;
Kreckel, Kathryn;
Kruijssen, J. M. Diederik;
Larson, Kirsten L.;
Lee, Janice C.;
Mayker, Ness;
McElroy, Rebecca;
Meidt, Sharon E.;
Mok, Angus;
Pan, Hsi-An;
Puschnig, Johannes;
Razza, Alessandro;
Sanchez-Blazquez, Patricia;
Sandstrom, Karin M.;
Santoro, Francesco;
Sardone, Amy;
Scheuermann, Fabian;
Sun, Jiayi;
Thilker, David A.;
Turner, Jordan A.;
Ubeda, Leonardo;
Utomo, Dyas;
Watkins, Elizabeth J.;
Williams, Thomas G.
The PHANGS-ALMA pipeline process data from radio interferometer observations. It uses CASA (ascl:1107.013), AstroPy (ascl:1304.002), and other affiliated packages to process data from calibrated visibilities to science-ready spectral cubes and maps. The PHANGS-ALMA pipeline offers a flexible alternative to the scriptForImaging script distributed by ALMA. The pipeline runs in two separate software environments: CASA 5.6 or 5.7 (staging, imaging and post-processing) and Python 3.6 or later (derived products) with modern versions of several packages.
[ascl:2203.016]
MaNGA-DRP: MaNGA Data Reduction Pipeline
Law, David R.;
Cherinka, Brian;
Yan, Renbin;
Andrews, Brett H.;
Bershady, Matthew A.;
Bizyaev, Dmitry;
Blanc, Guillermo A.;
Blanton, Michael R.;
Bolton, Adam S.;
Brownstein, Joel R.;
Bundy, Kevin;
Chen, Yanmei;
Drory, Niv;
D'Souza, Richard;
Fu, Hai;
Jones, Amy;
Kauffmann, Guinevere;
MacDonald, Nicholas;
Masters, Karen L.;
Newman, Jeffrey A.;
Parejko, John K.;
Sánchez-Gallego, José R.;
Sánchez, Sebastian F.;
Schlegel, David J.;
Thomas, Daniel;
Wake, David A.;
Weijmans, Anne-Marie;
Westfall, Kyle B.;
Zhang, Kai
The MaNGA Data Reduction Pipeline (DRP) processes the raw data to produce flux calibrated, sky subtracted, coadded data cubes from each of the individual exposures for a given galaxy. The DRP consists of two primary parts: the 2d stage that produces flux calibrated fiber spectra from raw individual exposures, and the 3d stage that combines multiple flux calibrated exposures with astrometric information to produce stacked data cubes. These science-grade data cubes are then processed by the MaNGA Data Analysis Pipeline (ascl:2203.017), which measures the shape and location of various spectral features, fits stellar population models, and performs a variety of other analyses necessary to derive astrophysically meaningful quantities from the calibrated data cubes.