1,721,017 research outputs found
Emil Lenc and Stewart Southam, Swinburne Astronomy Online Graduations, March 2009
No full textSwinburne Astronomy Online graduations, March 2009. Dr Emil Lenc (left) and Master Stewart Southam
Swinburne Astronomy Online Graduations, March 2004
No full textSwinburne Astronomy Online graduates, from left: Master Terence Dougherty (Australia), Dr Sarah Maddison (SAO), Master Emil Lenc (Australia), Dr Margaret Mazzolini (SAO) and Master Jan Barker (Australia), March 2004
Parkes observations for project P1320 semester 2024APRS_08
No full textYoung pulsars are critical for probing the early stages of neutron stars, offering insights into their initial spin periods, velocities, and luminosities. If they is present in supernova remnants (SNRs) then they also illuminate the broader phenomena of star deaths and the properties of supernovae. The proximity of a newly discovered pulsar PSR J1646-4451 to a potential SNR presents a unique opportunity to study the interplay between the pulsar and its surroundings. PSR J1646-4451 was first detected as a circularly polarized source in ASKAP's VAST survey in a close proximity of a likely SNR shell. In subsequent observations with the Ultra-Wideband Low (UWL) receiver system on the Parkes radio telescope (Murriyang), the source was confirmed as a pulsar with a spin period of 217 ms and a very high dispersion measure (DM) of 930 pc cm^-3. The pulsar is highly scattered and invisible below 2 GHz, meaning that UWL is the only instrument which can be used to study this interesting pulsar. The goal of this proposal is to measure the pulsar's characteristic age by conducting follow-up timing observations in 2024APRS. Determining the characteristic age of the pulsar is the first key step to establishing evidence for or against a possible association between the pulsar and the nearby SNR
Parkes observations for project P1320 semester 2024APRS_09
No full textYoung pulsars are critical for probing the early stages of neutron stars, offering insights into their initial spin periods, velocities, and luminosities. If they is present in supernova remnants (SNRs) then they also illuminate the broader phenomena of star deaths and the properties of supernovae. The proximity of a newly discovered pulsar PSR J1646-4451 to a potential SNR presents a unique opportunity to study the interplay between the pulsar and its surroundings. PSR J1646-4451 was first detected as a circularly polarized source in ASKAP's VAST survey in a close proximity of a likely SNR shell. In subsequent observations with the Ultra-Wideband Low (UWL) receiver system on the Parkes radio telescope (Murriyang), the source was confirmed as a pulsar with a spin period of 217 ms and a very high dispersion measure (DM) of 930 pc cm^-3. The pulsar is highly scattered and invisible below 2 GHz, meaning that UWL is the only instrument which can be used to study this interesting pulsar. The goal of this proposal is to measure the pulsar's characteristic age by conducting follow-up timing observations in 2024APRS. Determining the characteristic age of the pulsar is the first key step to establishing evidence for or against a possible association between the pulsar and the nearby SNR
Parkes observations for project P1320 semester 2024APRS_05
No full textYoung pulsars are critical for probing the early stages of neutron stars, offering insights into their initial spin periods, velocities, and luminosities. If they is present in supernova remnants (SNRs) then they also illuminate the broader phenomena of star deaths and the properties of supernovae. The proximity of a newly discovered pulsar PSR J1646-4451 to a potential SNR presents a unique opportunity to study the interplay between the pulsar and its surroundings. PSR J1646-4451 was first detected as a circularly polarized source in ASKAP's VAST survey in a close proximity of a likely SNR shell. In subsequent observations with the Ultra-Wideband Low (UWL) receiver system on the Parkes radio telescope (Murriyang), the source was confirmed as a pulsar with a spin period of 217 ms and a very high dispersion measure (DM) of 930 pc cm^-3. The pulsar is highly scattered and invisible below 2 GHz, meaning that UWL is the only instrument which can be used to study this interesting pulsar. The goal of this proposal is to measure the pulsar's characteristic age by conducting follow-up timing observations in 2024APRS. Determining the characteristic age of the pulsar is the first key step to establishing evidence for or against a possible association between the pulsar and the nearby SNR
New ASKAP images of the Abell 3627 cluster and the Corkscrew Galaxy
No full textThis collection contains new images from our paper entitled: "ASKAP reveals the radio tail structure of the Corkscrew Galaxy shaped by its passage through the Abell 3627 cluster". These are re-imaged ASKAP data products used in Koribalski et al. (2024, MNRAS, in press: https://arxiv.org/abs/2405.04374). The collection includes FITS images obtained after additional self-calibration and imaging of pre-calibrated data products retrieved from CASDA. The two SBIDs included are SB11816 (at 1367.5 MHz) and SB53218 (at 943.5 MHz), with images only covering the cluster Abell 3627 (Norma Cluster) instead of the full field of view. \n\nMaps of the position-dependent root-mean-square noise and spectral index maps derived from the images and described in the paper are also included. Images, DS9 region files, and tables associated with measurements of the spectral index in regions are also provided.\n\n The central effective frequency of each image is included in the file name, and the frequency range is included for spectral index maps. File names also typically include the image weighting, and “shift” in the filename indicates astrometric corrections have been applied as described in the paper. Files with “rgd” in their name are used for the corresponding spectral index maps after convolving images to a common resolution and regridding to a common image grid/projection. For more detail of the included images and the imaging procedure, please see the aforementioned paper.\
Parkes observations for project P1320 semester 2024APRS_06
No full textYoung pulsars are critical for probing the early stages of neutron stars, offering insights into their initial spin periods, velocities, and luminosities. If they is present in supernova remnants (SNRs) then they also illuminate the broader phenomena of star deaths and the properties of supernovae. The proximity of a newly discovered pulsar PSR J1646-4451 to a potential SNR presents a unique opportunity to study the interplay between the pulsar and its surroundings. PSR J1646-4451 was first detected as a circularly polarized source in ASKAP's VAST survey in a close proximity of a likely SNR shell. In subsequent observations with the Ultra-Wideband Low (UWL) receiver system on the Parkes radio telescope (Murriyang), the source was confirmed as a pulsar with a spin period of 217 ms and a very high dispersion measure (DM) of 930 pc cm^-3. The pulsar is highly scattered and invisible below 2 GHz, meaning that UWL is the only instrument which can be used to study this interesting pulsar. The goal of this proposal is to measure the pulsar's characteristic age by conducting follow-up timing observations in 2024APRS. Determining the characteristic age of the pulsar is the first key step to establishing evidence for or against a possible association between the pulsar and the nearby SNR
Parkes observations for project P1320 semester 2024APRS_04
No full textYoung pulsars are critical for probing the early stages of neutron stars, offering insights into their initial spin periods, velocities, and luminosities. If they is present in supernova remnants (SNRs) then they also illuminate the broader phenomena of star deaths and the properties of supernovae. The proximity of a newly discovered pulsar PSR J1646-4451 to a potential SNR presents a unique opportunity to study the interplay between the pulsar and its surroundings. PSR J1646-4451 was first detected as a circularly polarized source in ASKAP's VAST survey in a close proximity of a likely SNR shell. In subsequent observations with the Ultra-Wideband Low (UWL) receiver system on the Parkes radio telescope (Murriyang), the source was confirmed as a pulsar with a spin period of 217 ms and a very high dispersion measure (DM) of 930 pc cm^-3. The pulsar is highly scattered and invisible below 2 GHz, meaning that UWL is the only instrument which can be used to study this interesting pulsar. The goal of this proposal is to measure the pulsar's characteristic age by conducting follow-up timing observations in 2024APRS. Determining the characteristic age of the pulsar is the first key step to establishing evidence for or against a possible association between the pulsar and the nearby SNR
Going Beyond Counting First Authors in Author Co-citation Analysis
Get PDFThe present study examines one of the fundamental aspects of author co-citation analysis (ACA) - the way co-citation
counts are defined. Co-citation counting provides the data on which all subsequent statistical analyses and mappings
are based, and we compare ACA results based on two different types of co-citation counting - the traditional type that
only counts the first one among a cited work's authors on the one hand and a non-traditional type that takes into
account the first 5 authors of a cited work on the other hand. Results indicate that the picture produced through this non-traditional author co-citation counting contains more coherent author groups and is therefore considerably clearer. However, this picture represents fewer specialties in the research field being studied than that produced through the traditional first-author co-citation counting when the same number of top-ranked authors is selected and analyzed. Reasons for these effects are discussed
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