The Iraf Data Reduction And Analysis System

We provide timing solutions for 45 radio pulsars discovered by the Robert C. Byrd Green Bank Telescope. These pulsars were found in the Green Bank North Celestial Cap pulsar survey, an all-GBT-sky survey being carried out at a frequency of 350 MHz. We include pulsar timing data from the Green Bank Telescope and Low Frequency Array. Our sample includes five fully recycled millisecond pulsars (MSPs, three of which are in a binary system), a new relativistic double neutron star system, an intermediate-mass binary pulsar, a mode-changing pulsar, a 138 ms pulsar with a very low magnetic field, and several nulling pulsars. We have measured two post-Keplerian parameters and thus the masses of both objects in the double neutron star system. We also report a tentative companion mass measurement via Shapiro delay in a binary MSP. Two of the MSPs can be timed with high precision and have been included in pulsar timing arrays being used to search for low-frequency gravitational waves, while a third MSP is a member of the black widow class of binaries. Proper motion is measurable in five pulsars, and we provide an estimate of their space velocity. We report on an optical counterpart to a new black widow system and provide constraints on the optical counterparts to other binary MSPs. We also present a preliminary analysis of nulling pulsars in our sample. These results demonstrate the scientific return of long timing campaigns on pulsars of all types.

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“…sourceforge.net/), PINT (https://github.com/nanograv/PINT), IRAF (Tody 1986(Tody , 1993, SCAMP (Bertin & Arnouts 1996 …”

Section: Resultsmentioning

confidence: 99%

The Green Bank North Celestial Cap Pulsar Survey. III. 45 New Pulsar Timing Solutions

Lynch

Swiggum

Kondratiev

et al. 2018

ApJ

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“…We performed aperture photometry of SN 2012cg in a 0 4-diameter aperture using the hstsnphot 7 program used by the CLASH and CANDELS SN surveys (Graur et al 2014b;Rodney et al 2014), which is based on the IRAF 8 apphot routine (Tody 1986). Due to the faintness of the SN on the last observation epoch, 2015 April 26.6, we used a smaller aperture with a diameter of 0 24, along with a larger aperture correction, to capture the low flux counts.…”

Section: Discussionmentioning

confidence: 99%

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co

Graur

Zurek

Shara

et al. 2016

ApJ

103

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Seitenzahl et al. have predicted that roughly three years after its explosion, the light we receive from a Type Ia supernova (SN Ia) will come mostly from reprocessing of electrons and X-rays emitted by the radioactive decay chain 57 Co→ 57 Fe, instead of positrons from the decay chain 56 Co→ 56 Fe that dominates the SN light at earlier times. Using the Hubble Space Telescope, we followed the light curve of the SN Ia SN 2012cg out to 1055 days after maximum light. Our measurements are consistent with the light curves predicted by the contribution of energy from the reprocessing of electrons and X-rays emitted by the decay of 57 Co, offering evidence that 57 Co is produced in SN Ia explosions. However, the data are also consistent with a light echo ∼14 mag fainter than SN 2012cg at peak. Assuming no light-echo contamination, the mass ratio of 57 Ni and 56 Ni produced by the explosion, a strong constraint on any SN Ia explosion models, is 0.043 0.011 0.012 -+ , roughly twice Solar. In the context of current explosion models, this value favors a progenitor white dwarf with a mass near the Chandrasekhar limit.

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“…Data were reduced using the Image Reduction and Analysis Facility (IRAF) V2.14 noao longslit and Subaru focasred packages (Tody 1986). The reduction procedure included overscan and bias subtraction, image trimming, flattening, and cosmic ray removal for long exposure images.…”

Section: Data Reduction and Analysismentioning

confidence: 99%

Space weathering trends among carbonaceous asteroids

Kaluna

Masiero

Meech

2016

Icarus

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We present visible spectroscopic and albedo data of the 2.3 Gyr old Themis family and the <10 Myr old Beagle sub-family. The slope and albedo variations between these two families indicate C-complex asteroids become redder and darker in response to space weathering. Our observations of Themis family members confirm previously observed trends where phyllosilicate absorption features are less common among small diameter objects. Similar trends in the albedos of large (>15 km) and small (≤15 km) Themis members suggest these phyllosilicate feature and albedo trends result from regolith variations as a function of diameter. Observations of the Beagle asteroids show a small, but notable fraction of members with phyllosilicate features. The presence of phyllosilicates and the dynamical association of the main-belt comet 133P/Elst-Pizarro with the Beagle family imply the Beagle parent body was a heterogenous mixture of ice and aqueously altered minerals.Subject headings: main belt asteroids, carbonaceous asteroids, space weathering

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The Iraf Data Reduction And Analysis System

Cited by 1,483 publications

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The Green Bank North Celestial Cap Pulsar Survey. III. 45 New Pulsar Timing Solutions

The Green Bank North Celestial Cap Pulsar Survey. III. 45 New Pulsar Timing Solutions

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co

Space weathering trends among carbonaceous asteroids

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The Iraf Data Reduction And Analysis System

Cited by 1,483 publications

References 0 publications

The Green Bank North Celestial Cap Pulsar Survey. III. 45 New Pulsar Timing Solutions

The Green Bank North Celestial Cap Pulsar Survey. III. 45 New Pulsar Timing Solutions

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF 57Co

Space weathering trends among carbonaceous asteroids

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Product

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LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co