Access to Astronomical Catalogues

← Click to display the menu
J/ApJ/843/24  Hα interferometry obs. of the Be star 48 Per  (Jones+, 2017)

The disk physical conditions of 48 Persei constrained by contemporaneous Hα spectroscopy and interferometry. Jones C.E., Sigut T.A.A., Grzenia B.J., Tycner C., Zavala R.T. <Astrophys. J., 843, 24 (2017)> =2017ApJ...843...24J
ADC_Keywords: Stars, Be ; Interferometry Keywords: circumstellar matter; stars: emission-line, Be; stars: individual (48 Per); stars: massive; stars: mass-loss; techniques: interferometric; techniques: spectroscopic Abstract: We utilize a multi-step modeling process to produce synthetic interferometric and spectroscopic observables, which are then compared to their observed counterparts. Our extensive set of interferometric observations of the Be star 48 Per, totaling 291 data points, were obtained at the Navy Precision Optical Interferometer from 2006 November 07 to 23. Our models were further constrained by comparison with contemporaneous Hα line spectroscopy obtained at the John S. Hall Telescope at the Lowell Observatory on 2006 November 1. Theoretical spectral energy distributions, SEDs, for 48 Per were confirmed by comparison with observations over a wavelength regime of 0.4-60 µm from Touhami+ (2010PASP..122..379T) and Vieira+ (2017MNRAS.464.3071V). Our best-fitting combined model from Hα spectroscopy, Hα interferometry, and SED fitting has a power-law density fall off, n, of 2.3 and an initial density at the stellar surface of ρ0=1.0x10-11g/cm-3 with an inclination constrained by Hα spectroscopy and interferometry of 45±5°. The position angle for the system, measured east from north, is 114±18°. Our best-fit model shows that the disk emission originates in a moderately large disk with a radius of 25 R*, which is consistent with a disk mass of approximately 5x1024g or 3x10-10M*. Finally, we compare our results with previous studies of 48 Per by Quirrenbach+ (1997ApJ...479..477Q) and find agreement, whereas our disk size does not agree with Delaa+ (2011A&A...529A..87D), based on a much smaller visibility set. Description: Our observations of 48 Per were obtained at the Navy Precision Optical Interferometer (NPOI), located near Flagstaff, AZ, USA. Typically, observations from up to five unique baselines are obtained simultaneously; for this study, baseline lengths ranged from 18.9 to 64.4m. A total of 291 squared visibility measurements from a 150Å wide spectral channel containing the Hα emission line (i.e., centered at 6563Å) of 48 Per were obtained at NPOI in 2006 Nov 7-23. Objects: ------------------------------------------------------ RA (ICRS) DE Designation(s) ------------------------------------------------------ 04 08 39.69 +47 42 45.0 48 Per = TYC 3332-2427-1 ------------------------------------------------------ File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 45 291 Interferometric observations
See also: II/225 : Catalog of Infrared Observations, Edition 5 (Gezari+ 1999) II/224 : Catalogue of Stellar Diameters (CADARS) (Pasinetti-Fracassini+ 2001) I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007) J/A+A/290/609 : Be stars near-IR excess (Dougherty+, 1994) J/ApJ/689/461 : Circumstellar disk of χ Oph (Tycner+, 2008) J/AJ/139/2269 : P Cyg Hα squared visibility (Balan+, 2010) J/ApJ/814/159 : Hα interferometric visibilities of o Aqr (Sigut+, 2015) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 11 F11.3 d JD Observation Julian Date 13- 19 F7.3 10+6/rad u [-31.5/68.8] Spatial frequency u in 10+6cycles/radian 21- 27 F7.3 10+6/rad v [-31.6/87.2] Spatial frequency v in 10+6cycles/radian 29- 33 F5.3 --- VHa2 [0.5/1.1] Hα squared visibility 35- 39 F5.3 --- e_VHa2 [0.01/0.4] Uncertainty in VHa2 41- 45 A5 --- Baseline Baseline (1)
Note (1): The baselines AC-AE, AC-AW, AW-W7, AC-W7, AE-W7 correspond to lengths of 18.9, 22.2, 29.5, 51.6, and 64.4m, respectively.
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 05-Feb-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© Unistra/CNRS

Contact