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- This tutorial describes how to use CASA 5.5.0 to reduce spectral-line data in the low-frequency P-band of the VLA (230–470 MHz). The goal i * Additionally, if very high spectral dynamic range is needed (i.e., when expecting a ratio between the detection53 KB (7,864 words) - 12:50, 29 September 2020
- [[Category:EVLA]][[Category:Calibration]][[Category:Spectral Line]] This tutorial describes the data reduction for two spectral lines observed toward the Asymptotic Giant Branch (AGB) star [https://en.wi108 KB (16,776 words) - 15:14, 15 October 2020
- This tutorial describes how to use CASA 5.7.2 to reduce spectral-line data in the low-frequency P-band of the VLA (230–470 MHz). The goal i * Additionally, if very high spectral dynamic range is needed (i.e., when expecting a ratio between the detection57 KB (8,502 words) - 18:49, 22 December 2020
- #REDIRECT [[MG0414+0534 P-band Spectral Line Tutorial - CASA 6.5.4]]68 bytes (8 words) - 17:52, 29 February 2024
- [[Category:EVLA]][[Category:Calibration]][[Category:Spectral Line]] This tutorial describes the data reduction for two spectral lines observed toward the Asymptotic Giant Branch (AGB) star [https://en.wi119 KB (18,324 words) - 12:17, 24 February 2023
- This tutorial describes how to use CASA 6.2.0 to reduce spectral-line data in the low-frequency P-band of the VLA (230–470 MHz). The goal i * Additionally, if very high spectral dynamic range is needed (i.e., when expecting a ratio between the detection63 KB (9,411 words) - 23:23, 12 February 2023
- [[Category:EVLA]][[Category:Calibration]][[Category:Spectral Line]] This tutorial describes the data reduction for two spectral lines observed toward the Asymptotic Giant Branch (AGB) star [https://en.wi119 KB (18,324 words) - 14:03, 2 March 2023
- This tutorial describes how to use CASA 6.5.2 to reduce spectral-line data in the low-frequency P-band of the VLA (230–470 MHz). The goal i * Additionally, if very high spectral dynamic range is needed (i.e., when expecting a ratio between the detection66 KB (9,867 words) - 13:55, 24 January 2024
- #REDIRECT [[MG0414+0534 P-band Spectral Line Tutorial - CASA 6.5.2]]68 bytes (8 words) - 15:35, 13 February 2023
- [[Category:EVLA]][[Category:Calibration]][[Category:Spectral Line]] ...w to calibrate and image high-frequency (Ka Band) EVLA observations of two spectral lines toward the Asymptotic Giant Branch (AGB) star [https://en.wikipedia.o134 KB (19,330 words) - 16:53, 29 September 2023
- This tutorial describes how to use CASA 6.5.4 to reduce spectral-line data in the low-frequency P-band of the VLA (230–470 MHz). The goal i * Additionally, if very high spectral dynamic range is needed (i.e., when expecting a ratio between the detection66 KB (9,882 words) - 11:21, 29 February 2024
- This tutorial describes how to use CASA 6.5.4 to reduce spectral-line data in the low-frequency P-band of the VLA (230–470 MHz). The goal i * Additionally, if very high spectral dynamic range is needed (i.e., when expecting a ratio between the detection66 KB (9,882 words) - 14:06, 29 February 2024
- This tutorial describes the data reduction of the HI spectral line observed of the nearby (4.8 Mpc), gas-rich dwarf galaxy LEDA44055. For its ...rvation, a 16 MHz wide IF pair (A0C0 as seen in later in listobs) subband (spectral window, abbreviated as ''spw'' in CASA) using 4096 channels was observed, e79 KB (10,810 words) - 18:24, 14 February 2020
- This tutorial describes the data reduction of the HI spectral line observed of the nearby (4.8 Mpc), gas-rich dwarf galaxy LEDA44055. For its ...rvation, a 16 MHz wide IF pair (A0C0 as seen in later in listobs) subband (spectral window, abbreviated as ''spw'' in CASA) using 4096 channels was observed, e79 KB (10,809 words) - 14:21, 9 April 2021
- This tutorial describes the data reduction of the HI spectral line observed of the nearby (4.8 Mpc), gas-rich dwarf galaxy LEDA44055. For its ...rvation, a 16 MHz wide IF pair (A0C0 as seen in later in listobs) subband (spectral window, abbreviated as ''spw'' in CASA) using 4096 channels was observed, e85 KB (11,808 words) - 11:37, 2 May 2022
- This tutorial describes the data reduction of the HI spectral line observed of the nearby (4.8 Mpc), gas-rich dwarf galaxy LEDA44055. For its ...rvation, a 16 MHz wide IF pair (A0C0 as seen in later in listobs) subband (spectral window, abbreviated as ''spw'' in CASA) using 4096 channels was observed, e91 KB (12,686 words) - 20:32, 20 February 2024
- #REDIRECT [[HI 21cm (1.4 GHz) spectral line data reduction: LEDA 44055-CASA6.5.2]]82 bytes (10 words) - 19:27, 16 November 2022
Page text matches
- ...define to propose for ALMA observations (spatial resolution, sensitivity, spectral setup), and to let you play with the ALMA OT so that you feel comfortable e * If it is an emission/absorption line experiment, the width of the frequency structure that you want to detect (i15 KB (2,458 words) - 16:48, 7 June 2016
- == Continuum Subtraction for Line Emission == ...do not need to continuum subtract if the line of interest is an absorption line.16 KB (2,477 words) - 16:36, 28 February 2024
- [[Category:ALMA]][[Category:Calibration]][[Category:Spectral Line]] ...duction and imaging of ALMA Science Verification data targeting the CO 3-2 line in the Antennae galaxy. These data were obtained using the ALMA Band 7 rece9 KB (1,443 words) - 12:08, 22 November 2011
- [[Category:ALMA]][[Category:Calibration]][[Category:Spectral Line]] available basebands, which are associated with four different spectral windows: two9 KB (1,395 words) - 09:09, 7 September 2015
- ...t look at spectral line imaging]]: This guide shows imaging of a spectral line. ...t spectral line imaging in CASA]]: This guide shows imaging of a spectral line.8 KB (1,160 words) - 16:55, 13 May 2024
- [[Category:ALMA]][[Category:Calibration]][[Category:Spectral Line]] ...u/abs/2005ApJ...622.1171R Roberge et al. 2005]; Figure 7). The solid green line is the direction of maximum disk brightness at optical wavelengths.]]9 KB (1,372 words) - 22:05, 9 January 2017
- ** [[Selecting Spectral Windows and Channels]] ** <big> [http://www.splatalogue.net Splatalogue - Astronomical Line Database] </big>3 KB (404 words) - 00:19, 18 November 2017
- * A first look at spectral line imaging: [[First_Look_at_Line_Imaging_4.4 | CASA 4.4]] [[First_Look_at_Line2 KB (320 words) - 17:19, 12 October 2023
- == Continuum Subtraction for Line Emission == ...do not need to continuum subtract if the line of interest is an absorption line.16 KB (2,499 words) - 15:03, 18 October 2023
- [[Category:ALMA]][[Category:Calibration]][[Category:Spectral Line]] ...duction and imaging of ALMA Science Verification data targeting the CO 3-2 line in the Antennae galaxy. These data were obtained using the ALMA Band 7 rece10 KB (1,605 words) - 11:54, 30 May 2012
- The first few tutorials provided us with a spectral line data cube and a continuum image. Next we'd like to ...e extracted script and you want to use your own images from completing the line imaging tutorial12 KB (1,674 words) - 10:15, 8 February 2024
- ...data table is arranged so that each row is a single timestamp for a single spectral window and a single baseline. There are several columns. DATA holds the ori * {{uvcontsub}}: carry out uv-plane continuum subtraction for spectral-line data6 KB (862 words) - 17:03, 27 March 2013
- This tutorial picks up where [[EVLA Spectral Line Calibration IRC+10216]] leaves off. [[Image:irc10216_uvspec.png|thumb|UV-plot of the spectral line signal in both spw for IRC+10216.]]21 KB (3,516 words) - 16:03, 2 September 2011
- ...he MS (see example below) as well as estimate the zenith opacity for each spectral window. This script is only intended for use with the EVLA-- it contains h #edit the last line of the script, replacing MSname.ms with the name of your measurement set, a2 KB (344 words) - 13:26, 13 December 2012
- ...s here (about 15 MHz per channel). The spectral windows cover the CO J=1-0 line, a CN doublet, and the 3mm continuum. All three types of emission are visib ...ode) and cover the 850 micron continuum, the CO J=3-2 line, and HCO+ J=4-3 line. There is a full CASA Guide describing the reduction and imaging of these d21 KB (3,592 words) - 16:03, 26 February 2013
- ...as the first argument in order to determine the center frequencies of each spectral window. (To avoid the need for this file in the future, we have submitted ...y, it produces a plot summarizing the results. By default, it will use all spectral windows, but it will exclude those with an "INSUFFICIENT DATA" status from8 KB (1,058 words) - 12:56, 8 August 2013
- ...ctral Line tutorial - IRC+10216 part1]] and [[EVLA high frequency Spectral Line tutorial - IRC+10216 part2]]. [[Category:EVLA]][[Category:Calibration]][[Category:Spectral Line]]13 KB (1,838 words) - 17:57, 6 January 2012
- ...ctral Line tutorial - IRC+10216 part1]] and [[EVLA high frequency Spectral Line tutorial - IRC+10216 part2]]. [[Category:EVLA]][[Category:Calibration]][[Category:Spectral Line]]13 KB (1,853 words) - 13:35, 9 January 2012
- ...mes the bandpass calibrator at the required frequency is contaminated with line absorption or emission. In particular, this is notorious for observations c ...bserving frequency. The offset frequencies should be chosen clean from any line contamination, but with as little frequency offset as possible. Ideally it10 KB (1,205 words) - 15:47, 11 March 2021
- ...iate amount of channel averaging has been applied to reduce the data size. Line data sets are provided at their full resolution. If self-calibration was po ...the primary beam images themselves and can be applied to the corresponding line data if desired using the CASA task {{impbcor}}.16 KB (2,452 words) - 10:11, 8 May 2018
