J/A+A/625/A66 X-ray data for 56 protoplanetary disk sources (Dionatos+ 2019)
Consistent dust and gas models for protoplanetary disks.
IV. A panchromatic view of protoplanetary disks.
Dionatos O., Woitke P., Guedel M., Degroote P., Liebhart A., Anthonioz F.,
Antonellini S., Baldovin-Saavedra C., Carmona A., Dominik C., Greaves J.,
Ilee J.D., Kamp I., Menard F., Min M., Pinte C., Rab C., Rigon L.,
Thi W.F., Waters L.B.F.M.
<Astron. Astrophys. 625, A66 (2019)>
=2019A&A...625A..66D 2019A&A...625A..66D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, pre-main sequence; Accretion; Spectroscopy; X-ray sources
Keywords: stars: formation - circumstellar matter - stars: variables: T Tauri -
Herbig Ae/Be - accretion - accretion disks -
astronomical databases: miscellaneous
Abstract:
Consistent modeling of protoplanetary disks requires the simultaneous
solution of both continuum and line radiative transfer, heating and
cooling balance between dust and gas and, of course, chemistry. Such
models depend on panchromatic observations that can provide a complete
description of the physical and chemical properties and energy balance
of protoplanetary systems. Along these lines we present a homogeneous,
panchromatic collection of data on a sample of 85 T Tauri and Herbig
Ae objects for which data cover a range from X-rays to centimeter
wavelengths. Datasets consist of photometric measurements, spectra,
along with results from the data analysis such as line fluxes from
atomic and molecular transitions. Additional properties resulting from
modeling of the sources such as disc mass and shape parameters, dust
size and PAH properties are also provided for completeness.
The purpose of this data collection is to provide a solid base that
can enable consistent modeling of the properties of protoplan- etary
disks. To this end, we performed an unbiased collection of publicly
available data that were combined to homogeneous datasets adopting
consistent criteria. Targets were selected based on both their
properties but also on the availability of data.
Data from more than 50 different telescopes and facilities were
retrieved and combined in homogeneous datasets directly from public
data archives or after being extracted from more than 100 published
articles. X-ray data for a subset of 56 sources represent an exception
as they were reduced from scratch and are presented here for the first
time.
Compiled datasets along with a subset of continuum and emission-line
models are stored in a dedicated database and distributed through a
publicly accessible online system. All datasets contain metadata
descriptors that allow to backtrack them to their original resources.
The graphical user interface of the online system allows the user to
visually inspect individual objects but also compare between datasets
and models. It also offers to the user the possibility to download any
of the stored data and metadata for further processing.
Description:
We present X-ray data from 56 T Tauri and Herbig Ae sources collected
and reduced for the purposes of the DiscAnalysis (DIANA) project. Data
were obtained with XMM-Newton and Chandra missions and are presented
in xray_obs.dat. Data were further modeled using the XSPEC package
(Arnaud+ 1996) where and n-temperature component (n=1-3) was fit to
the data. The fit delivers the absorption column density, plasma
emission temperatures and hardness that are presented in Table 4.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
xray_obs.dat 62 56 List of X-ray observations
table4.dat 126 55 Model results of X-ray spectra
(corrected version, 18-May-2021)
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Byte-by-byte Description of file: xray_obs.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Source name
10- 11 I2 h RAh Right ascension (J2000.0)
13- 14 I2 min RAm Right ascension (J2000.0)
16- 19 F4.1 s RAs Right ascension (J2000.0)
21 A1 --- DE- Declination sign (J2000.0)
22- 23 I2 deg DEd Declination (J2000.0)
25- 26 I2 arcmin DEm Declination (J2000.0)
28- 31 F4.1 arcsec DEs Declination (J2000.0)
33- 42 A10 --- Inst Instrument (XMM-Newton or Chandra)
44- 53 I10 --- ObsId Observation identification
55- 62 F8.1 sec IntTime Integration time (seconds)
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Source name
10- 11 I2 h RAh Right ascension (J2000.0)
13- 14 I2 min RAm Right ascension (J2000.0)
16- 19 F4.1 s RAs Right ascension (J2000.0)
21 A1 --- DE- Declination sign (J2000.0)
22- 23 I2 deg DEd Declination (J2000.0)
25- 26 I2 arcmin DEm Declination (J2000.0)
28- 31 F4.1 arcsec DEs Declination (J2000.0)
33- 40 E8.2 cm-2 CD Column Density
42- 49 E8.2 mW/m2 Flux Flux
51- 58 E8.2 mW/m2 FluxS Flux soft
60- 67 E8.2 mW/m2 FluxH Flux hard
69- 74 F6.3 --- h1 Hardness
76- 83 E8.2 mW/m2 Fabs Flux absorbed
85- 92 E8.2 mW/m2 FabsS Flux absorbed soft
94-101 E8.2 mW/m2 FabsH Flux absorbed hard
103-108 F6.3 --- h2 Hardness absorbed
110-117 E8.2 K T1 Temperature component 1
119-126 E8.2 K T2 Temperature component 2
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Acknowledgements:
Odysseas Dionatos, odysseas.dionatos(at)univie.ac.at
www.univie.ac.at/diana
References:
Woitke et al., Paper I 2016A&A...586A.103W 2016A&A...586A.103W
Kamp et al., Paper II 2017A&A...607A..41K 2017A&A...607A..41K
History:
14-May-2019: on-line version
18-May-2021: in table4.dat, exponents of fluxes corrected
(End) O. Dionatos [Univ. Vienna, Austria], P. Vannier [CDS] 07-Mar-2019