A listing of the various RFI in this frequency band is available here.

Also available are spectra per 128 MHz subband.

CSV files for RR and LL - 10/10

CSV files for RR and LL - 11/21

CSV files for RR and LL - 11/25

CSV files for RR and LL - 11/25

CSV files for RR and LL - 12/02

CSV files for RR and LL - 12/12

CSV files for RR and LL - 12/12

CSV files for RR and LL - 01/06

CSV files for RR and LL - 01/06

CSV files for RR and LL - 01/21

CSV files for RR and LL - 02/10

CSV files for RR and LL - 02/10

CSV files for RR and LL - 02/24

CSV files for RR and LL - 02/24

A listing of the various RFI in this frequency band is available here.

Also available are spectra per 128 MHz subband.

CSV files for RR and LL - 03/13

CSV files for RR and LL - 03/13

CSV files for RR and LL - 03/24

CSV files for RR and LL - 03/24

CSV files for RR and LL - 04/07

CSV files for RR and LL - 04/07

CSV files for RR and LL - 04/24

CSV files for RR and LL - 04/24

CSV files for RR and LL - 05/05

CSV files for RR and LL - 05/05

A listing of the various RFI in this frequency band is available here.

Also available are spectra per 128 MHz subband.

CSV files for RR and LL - 03/13

CSV files for RR and LL - 03/13

CSV files for RR and LL - 03/24

CSV files for RR and LL - 03/24

CSV files for RR and LL - 04/07

CSV files for RR and LL - 04/07

CSV files for RR and LL - 04/24

CSV files for RR and LL - 04/24

CSV files for RR and LL - 05/05

CSV files for RR and LL - 05/05

A listing of the various RFI in this frequency band is available here.

Also available are spectra per 128 MHz subband.

CSV files for RR and LL - 03/13

CSV files for RR and LL - 03/13

CSV files for RR and LL - 03/24

CSV files for RR and LL - 03/24

CSV files for RR and LL - 04/07

CSV files for RR and LL - 04/07

CSV files for RR and LL - 04/24

CSV files for RR and LL - 04/24

CSV files for RR and LL - 05/05

CSV files for RR and LL - 05/05

May 9, 2025

11:00am Mountain

Alice Harding (LANL)

Pulsars in the High-Energy Sky

Abstract

Of the several thousand pulsars that have been discovered by radio telescopes over the past fifty years, only a handful were known to emit gamma-ray pulsations before the launch in June, 2008 of the Fermi Gamma-Ray Space Telescope. After 17 years of operation, over 300 gamma-ray pulsars have been detected and a new population of radio-quiet pulsars has been discovered. Millisecond pulsars have been confirmed as powerful sources of gamma-ray emission, and a whole population of these objects is seen with Fermi both in the Galactic plane and in globular clusters. A gamma-ray pulsar timing array (PTA) using millisecond pulsars is now operating and may soon independently detect the gravitational wave background recently discovered by radio PTAs. Fermi has thus revolutionized the study of pulsars and allowed us to peer deeper into the inner workings of these incredibly efficient natural particle accelerators. These discoveries, together with recent progress in global simulation of pulsar magnetospheres, are changing our models of pulsar particle acceleration and high-energy as well as coherent radio emission..

Local Host: Dale Frail

The NSF National Radio Astronomy Observatory, NSF Green Bank Observatory, Central Development Laboratory, and Associated Universities, Inc. will be playing a major part in the January 2026 247th meeting of the American Astronomical Society.  Join the NSF NRAO leadership, staff, users, and students for a week sharing outstanding science results, press conferences, and technology developments.

Visit the NRAO in the exhibit hall, starting with the opening reception on Sunday evening.  Learn about the ALMA Wideband Sensitivity Upgrade, the ngVLA prototype antenna, new opportunities with the Green Bank Telescope and Dysh, and capabilities for observing with the VLA and VLBA from New Mexico Operations.  Join the NRAO leadership for the NRAO Town Hall evening on Tuesday, January 6th to learn about the latest research and development initiatives.

See the meeting website for conference details.

The block schedule is available on the AAS Website.

Pre-register for the Synthesis Imaging Workshop, May 2026.

Each link in the list below presents scalar-averaged cross correlation spectra using several baselines in the C-configuration for each respective receiver band obtained in 2025's C-configuration. The channel separation is 125 kHz. The antennas are pointed to the north celestial pole and away from known RFI sources. Hanning smoothing has been applied to minimize Gibbs ringing. The scale is logarithmic, in dB, with arbitrary offset. The scale can be roughly calibrated by noting that the mean power level is roughly equal to the antenna SEFD in Jy. There is no bandpass calibration, so the downturns at the edges are due to the analog and/or digital filters.

In addition, each link contains .CSV files. These files contain the values needed to plot Amplitude vs Frequency for the RR and LL correlations. Similar to the above, the values are scalar-averaged cross correlations, Hanning smoothing has been applied, and no bandpass calibration has been performed. The amplitudes are in Janskys calibrated using the system temperature of the antennas. Due to the gain compression effect the reported values are better thought of as lower limits than absolute fluxes of the RFI.

• P-Band (224-480 MHz)
• L-Band (1-2 GHz)
• S-Band (2-4 GHz)
• C-Band (4-8 GHz)
• X-Band (8-12 GHz)
• Ku-Band (12-18 GHz)
• K-Band (18-26.5 GHz)
• Ka-Band (26.5-40 GHz)
• Q-Band (40-50 GHz)

A listing of the various RFI in this frequency band is available here.

Also available are spectra per 16 MHz subband.

CSV files for RR and LL - 05/27

CSV files for RR and LL - 05/29

CSV files for RR and LL - 06/09

CSV files for RR and LL - 06/09

CSV files for RR and LL - 06/26

CSV files for RR and LL - 06/26

CSV files for RR and LL - 07/24

CSV files for RR and LL - 07/24

CSV files for RR and LL - 08/04

CSV files for RR and LL - 08/04

A listing of the various RFI in this frequency band is available here.

Also available are spectra per 16 MHz subband.

CSV files for RR and LL - 08/18

CSV files for RR and LL - 08/18

CSV files for RR and LL - 09/11

CSV files for RR and LL - 09/11

CSV files for RR and LL - 09/18

CSV files for RR and LL - 09/29

CSV files for RR and LL - 09/29

CSV files for RR and LL - 10/16

CSV files for RR and LL - 10/16

A listing of the various RFI in this frequency band is available here.

Also available are spectra per 128 MHz subband.

CSV files for RR and LL - 08/18

CSV files for RR and LL - 08/18

CSV files for RR and LL - 09/11

CSV files for RR and LL - 09/11

CSV files for RR and LL - 09/18

CSV files for RR and LL - 09/29

CSV files for RR and LL - 09/29

CSV files for RR and LL - 10/16

CSV files for RR and LL - 10/16

Wednesday Lunch is a rather informal lunchtime get-together with pizza to hear visitors' results as well as what staff are doing. If you or one of your visitors would like to speak at Wednesday Lunch, please contact Dillon Dong (username ddong) at username@nrao.edu.

Wednesday Lunch is held in the auditorium of the Domenici Science Operations Center (DSOC) in Socorro, New Mexico from noon until 1:00 PM unless indicated. All are welcome.

Wednesday Lunch schedules from previous years

Other Astrophysics Colloquia

• NRAO Socorro Colloquia
• NRAO Charlottesville Colloquia
• NRAO Charlottesville Lunch Seminar (TUNA)
• NRAO Green Bank Colloquia

• NMT Physics Dept. Colloquia (Socorro, NM)
• UNM Physics & Astronomy Dept. Colloquia (Albuquerque, NM)
• NMSU Astronomy Dept. Colloquia (Las Cruces, NM)

File contents

# This CASA pipescript is meant for use with CASA 6.6.6 and pipeline 2025.1.0.32
context = h_init()
context.set_state('ProjectSummary', 'observatory', 'Karl G. Jansky Very Large Array')
context.set_state('ProjectSummary', 'telescope', 'EVLA')
try:
    hifv_importdata(vis=['myCaldMS.ms'], datacolumns={'data': 'raw','corrected': 'regcal_contline_all'})
    hifv_flagtargetsdata()
    hifv_mstransform()
    hif_checkproductsize(maximsize=16384)
    hif_makeimlist(specmode='cont', datatype='regcal')
    hif_makeimages(hm_cyclefactor=3.0)
    hif_selfcal()
    hif_makeimlist(specmode='cont', datatype='selfcal')
    hif_makeimages(hm_cyclefactor=3.0)    
    hifv_exportdata(imaging_products_only=True)
finally:
    h_save()