J/ApJS/271/23 The Arecibo Observatory 327MHz (AO327) pulsars (Deneva+, 2024)
The AO327 drift survey catalog and Data Release of pulsar detections.
Deneva J.S., McLaughlin M., Olszanski T.E.E., Lewis E.F., Pang D.,
Freire P.C.C., Bagchi M., Stovall K.
<Astrophys. J. Suppl. Ser., 271, 23 (2024)>
=2024ApJS..271...23D 2024ApJS..271...23D
ADC_Keywords: Pulsars; Radio sources; Surveys
Keywords: Pulsars ; Neutron stars ; Catalogs ; Surveys
Abstract:
The AO327 drift survey for radio pulsars and transients used the
Arecibo telescope from 2010 until its collapse in 2020. AO327
collected ∼3100hr of data at 327MHz with a time resolution of 82µs
and a frequency resolution of 24kHz. While the main motivation for
such surveys is the discovery of new pulsars and new, even unforeseen,
types of radio transients, they also serendipitously collect a wealth
of data on known pulsars. We present an electronic catalog of data and
data products of 206 pulsars whose periodic emission was detected by
AO327 and are listed in the Australia Telescope National Facility
catalog of all published pulsars. The AO327 data products include
dedispersed time series at full time resolution, average ("folded")
pulse profiles, Gaussian pulse profile templates, and an absolute
phase reference that allows phase aligning the AO327 pulse profiles in
a physically meaningful manner with profiles from data taken with
other instruments. We also provide machine-readable tables with
uncalibrated flux measurements at 327 MHz and pulse widths at 50% and
10% of the pulse peak determined from the fitted Gaussian profile
templates. The AO327 catalog data set can be used in applications like
population analysis of radio pulsars, pulse profile evolution studies
in time and frequency, cone and core emission of the pulsar beam,
scintillation, pulse intensity distributions, and others. It also
constitutes a ready-made resource for teaching signal-processing and
pulsar astronomy techniques.
Description:
The AO327 drift survey for pulsars and transients operated from 2010
to 2020 and was cut short when the Arecibo telescope collapsed.
From 2010 February 10 to 2014 March 16 we used the Mock spectrometer,
and from 2014 March 17 to 2020 August 8 we used the newer Puerto
Rico Ultimate Pulsar Processing Instrument (PUPPI) backend.
We recorded data from the 2816 channels covering the usable 68.75MHz
bandwidth of the 327MHz receiver.
See Section 2.
The AO327 survey has detected 206 known pulsars listed in the ATNF
catalog as periodic emitters.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 57 19 Pulsar parameters from the ATNF catalog and
improved values from AO327 data
table2.dat 52 206 Pulse widths W and fractional duty cycles
table3.dat 79 213 *List of pulsar detections
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Note on table3.dat: Some detections made outside the main beam are not shown
in this table, although they appear in Table 2 (e.g. B0531+21 and
B0751+32). We do not report flux density estimates for those cases as
they are not covered by the representation of the main beam gain in
Equation 2.
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See also:
B/psr : ATNF Pulsar Catalogue (Manchester+, 2005)
J/ApJS/121/171 : Arecibo polarimetry of 98 pulsars (Weisberg+, 1999)
J/ApJ/605/759 : Multifrequency obs. of radio pulse broadening (Bhat+, 2004)
J/MNRAS/359/1524 : 10 new pulsars in Arecibo drift-scan survey (Lorimer+, 2005)
J/MNRAS/436/3557 : Long-period pulsars polarimetry (Tiburzi+, 2013)
J/ApJ/804/23 : 327MHz observations of 124 pulsars (Krishnakumar+, 2015)
J/ApJ/812/81 : Arecibo Pulsar-ALFA (PALFA) survey. IV. (Lazarus+, 2015)
J/MNRAS/489/1543 : Arecibo polarimetric single-pulse survey (Olszanski+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- PSR Pulsar name
13- 14 A2 --- Param Parameter (P=period or DM=Dispersion Measure)
16- 22 A7 --- x_Param Unit for Parameter
24- 31 F8.4 --- ATNF [0.09/188] Pulsar parameter from ATNF catalog
33- 37 F5.2 --- e_ATNF [0.03/30]? Uncertainty in ATNF
39- 48 F10.6 --- AO327 [0.36/184.1] Pulsar parameter from AO327 data
50- 57 F8.6 --- e_AO327 [3.2e-05/0.5]? Uncertainty in AO327
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- PSR Pulsar Name
13- 20 F8.6 s Per [0.002/6.3] Period (1)
22- 27 F6.2 pc/cm3 DM [3/314.4] Dispersion Measure (1)
29- 33 F5.1 ms W50 [0.2/278.6] Pulse width, 50% highest pulse
peak (2)
35- 40 F6.1 ms W10 [0.3/1018.4] Pulse width, 10% highest pulse
peak (2)
42- 46 F5.3 --- DC50 [0.004/0.43] Fractional duty cycle, 50% highest
pulse peak (2)
48- 52 F5.3 --- DC10 [0.008/0.87] Fractional duty cycle, 10% highest
pulse peak (2)
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Note (1): The Per and DM columns contain values from the ATNF catalog
except for the pulsars and respective parameters listed in Table 1;
in those cases the improved AO327 values are included here.
Note (2): Pulse widths W and fractional duty cycles DC at 50% and 10%
of the highest pulse peak, as determined from the single- or
multi-Gaussian template fitted to the folded pulse profile of each
pulsar. For pulsars with more than one detection the template was
fitted to the folded pulse profile of the detection with the
highest signal-to-noise.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- PSR Pulsar Name
13- 17 I5 d MJD [56759/59069] Modified Julian Date
(JD-2400000.5)
19- 53 A35 --- FileName Raw data file basename
55- 58 F4.2 arcmin Y [0.01/8.6] Angular offset, pulsar and beam
center (1)
60- 63 F4.2 --- EPS [0.35/0.9] Gain correction factor
65- 68 F4.2 mJy Smin [0.14/2.2] 6σ detection threshold
70- 74 F5.1 mJy S [0.4/223.3] Uncalibrated flux density (2)
76- 79 F4.1 mJy e_S [0.2/28] Uncertainty in S (2)
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Note (1): Angular offset between the pulsar and beam center in declination in
arcminutes.
Note (2): The uncalibrated flux density S, and flux density uncertainty e_S
are calculated separately for each detection since they depend on the
pulsar's track through the beam.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 17-Jun-2024