J/ApJ/918/71 Spitzer/IRAC photometry of V488 Persei debris disk (Rieke+, 2021)
Extreme variability of the V488 Persei debris disk.
Rieke G.H., Su K.Y.L., Melis C., Gaspar A.
<Astrophys. J., 918, 71 (2021)>
=2021ApJ...918...71R 2021ApJ...918...71R
ADC_Keywords: YSOs; Photometry, infrared; Stars, variable
Keywords: Debris disks ; Exoplanet migration
Abstract:
V488 Persei is the most extreme debris disk known in terms of the
fraction of the stellar luminosity it intercepts and reradiates. The
infrared output of its disk is extremely variable, similar in this
respect to the most variable disk known previously, that around ID8 in
NGC 2547. We show that the variations are likely to be due to
collisions of large planetesimals (≳100km in diameter) in a belt
being stirred gravitationally by a planetary or low-mass-brown-dwarf
member of a planetary system around the star. The dust being produced
by the resulting collisions is falling into the star due to drag by
the stellar wind. The indicated planetesimal destruction rate is so
high that it is unlikely that the current level of activity can
persist for much longer than ∼1000-10000yr and it may signal a major
realignment of the configuration of the planetary system.
Description:
V488 Per had two ∼45 days visibility windows every year for Spitzer,
separated by ∼120 days. We report in Figure 1 Spitzer/IRAC warm
mission observations made under programs 11093, 13014, and 14226 from
2015 April through the end of the mission in early 2020, providing a
total time baseline of ∼1800 days. All observations used both the
3.6 and 4.5um IRAC wave bands (IRAC1 and IRAC2). Sampling frequencies
were typically once per three days.
Furthermore, V488 Per was observed once with IRAC (AOR 18853632,
PID: 30717) during the Spitzer cold mission as reported by
Zuckerman+ (2012, J/ApJ/752/58). For consistency, we also conducted
our own photometry on these data.
We collected all WISE measurements from the NASA/IPAC Infrared Science
Archive where single exposure source catalogs are available through
different phases of the WISE mission (WISE All Sky Database, WISE
3-Band Cryo Database, and NEOWISE Reactivation Database).
To study the variability of V488 Per, we have used optical V-band
photometry from the AAVSO and ASAS-SN archives, plus measurements
specifically obtained for this program with Super-LOTIS (Livermore
Optical Transient Imaging System), a robotic telescope dedicated to
the search for optical counterparts of gamma-ray bursts (GRBs) and
located at the Steward Observatory Kitt Peak site. See Section 2.2.2.
Photometry of V488 Per using intermediate-band filters around 10um was
obtained with the Cooled Mid-Infrared Camera and Spectrometer (COMICS)
on the Subaru Telescope on 2017 January 14 and 2018 January 28
(BMJD-57120 of 648 and 1027, respectively).
Herschel PACS 70 and 160um observations were obtained in
2012-September-11 (PID OT2cmelis3, OBSID 1342250847 and 1342250848).
We retrieved the archival data from the Herschel Science Center.
See Section 2.3.2.
Prosser+ (1996AJ....112.1570P 1996AJ....112.1570P) report an X-ray detection of V488 Per
with the ROSAT Position Sensitive Proportional Counter (PSPC).
See Section 2.3.4.
Objects:
-------------------------------------------------------------------
RA (ICRS) DE Designation(s)
-------------------------------------------------------------------
03 28 18.68 +48 39 48.1 V488 Per = Gaia DR3 249236647249997696
-------------------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 58 129 Spitzer IRAC 3.6um and 4.5um IRAC wave bands
(IRAC1 and IRAC2) photometry of V488 Per
--------------------------------------------------------------------------------
See also:
V/80 : Low-Mass Stars' Membership in Alpha Persei Cluster (Prosser 1992)
J/A+A/411/559 : Effective temperature for 181 F-K dwarfs (Kovtyukh+, 2003)
J/AJ/132/161 : NStars project: The southern sample. I. (Gray+, 2006)
J/AJ/131/2967 : α Persei open cluster members (Makarov+, 2006)
J/ApJ/670/516 : NGC 2547 4.5-8um photometry (Gorlova+, 2007)
J/A+A/488/409 : Radial velocities of α Per stars (Mermilliod+, 2008)
J/ApJ/698/1989 : Spitzer survey of NGC 2451 (Balog+, 2009)
J/ApJ/745/147 : Binaries among debris disk stars (Rodriguez+, 2012)
J/ApJ/752/58 : α Per cluster members (Zuckerman+, 2012)
J/ApJ/768/25 : Spitzer & Herschel obs. of debris disks (Gaspar+, 2013)
J/ApJS/208/9 : Intrinsic colors & temperatures of PMS stars (Pecaut+, 2013)
J/ApJ/788/48 : X-ray through NIR photometry of NGC 2617 (Shappee+, 2014)
J/A+A/575/A18 : Revising the ages of planet-hosting stars (Bonfanti+, 2015)
J/ApJ/805/77 : Spitzer 3.6 and 4.5um monitoring of 5 stars (Meng+, 2015)
J/MNRAS/449/3160 : Stellar multiplicity and debris discs (Rodriguez+, 2015)
J/ApJ/823/108 : A dust model for bet Pic from 0.58-870um (Ballering+, 2016)
J/ApJ/836/34 : 24um obs. in clusters & membership of NGC2244 (Meng+, 2017)
J/A+A/618/A93 : Gaia DR2 open clusters in the MW (Cantat-Gaudin+, 2018)
J/AJ/156/241 : Variable stars measured by ATLAS (Heinze+, 2018)
J/AJ/158/93 : Regression of stellar Teff in GaiaDR2 (Bai+, 2019)
J/AJ/157/202 : IRAC fluxes of the ID8 and P1121 systems (Su+, 2019)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- AOR Spitzer AOR key
10- 20 F11.5 d BMJD1 [54004.27/58874.65] Barycentric modified Julian
Date of F3.6 observation
22- 27 F6.3 mJy F3.6 [27.65/86.9] Spitzer/IRAC 3.6um band flux density
29- 33 F5.3 mJy e_F3.6 [0.1/0.63] Uncertainty in F3.6
35- 45 F11.5 d BMJD2 [54004.26/58874.65] Barycentric modified Julian
Date of F4.5 observation
47- 52 F6.3 mJy F4.5 [26.34/96.21] Spitzer/IRAC 4.5um band flux density
54- 58 F5.3 mJy e_F4.5 [0.048/4.2] Uncertainty in F4.5
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 16-Jan-2023