High Resolution X-Ray Spectra A DIAGNOSTIC TOOL OF THE HOT UNIVERSE

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Presentation transcript:

High Resolution X-Ray Spectra A DIAGNOSTIC TOOL OF THE HOT UNIVERSE Katarzyna Bensch Rosario González-Riestra María Santos-Lleó XMM-NEWTON / ESAC

The RGS Instruments 18000 RGS SPECTRA 9000 OBSERVATIONS THE REFLECTION GRATING SPECTROMETER HIGH RESOLVING POWER: 7 TO 38 Å [~ 0.33-2.5 keV] SIMULTANEOUS OBSERVATIONS WITH EPIC AND OM 18000 RGS SPECTRA 9000 OBSERVATIONS RGS DESIGNED TO STUDY X-RAY EMISSION & ABSORPTION K-SHELL TRANSITION HELIUM-LIKE TRIPLETS OF C, N, O, Ne, Si, Ar L-SHELL TRANSITION of Fe DIAGNOSATIC TOOLS TO STUDY THE X-RAY SOURCES The X-ray Universe 2014

Work 1. Identification of useful Spectra FITTING THE SPATIAL PROFILES 2. Classification of spectra: FITTING THE SPATIAL PROFILES QUALITY TOP QUALITY / LOWER QUALITY SPATIAL EXTENT POINT-LIKE SOURCES / EXTENDED SOURCES The X-ray Universe 2014 The X-ray Universe 2014

BiRD Browsing Interface for RGS Data START POINT: BiRD DATABASE ALL PUBLIC RGS 1 & RGS 2 Events file + spectra EACH ONE HAS ASSOCIATED: Simbad Object Class, Nh, z / vrad http://xmm.esac.esa.int/BiRD/ The X-ray Universe 2014

Identification of useful Spectra Fitting Gaussian function to cross-dispersion profiles Statistically bad fit = discarded | except... Seyfert 1 Galaxy The X-ray Universe 2014

Identification of useful Spectra FITTING GAUSSIAN TO CROSS-DISPERSION PROFILE BiRD EVENTS FILES CALCULATING FLUX & ASSOCIATED ERROR BIRD SPECTGRA Defining “minimum usability” Parameters FWHM > 3∆FWHM FWHM ≥ INTRINSIC RESOLUTION INTENSITY > 3∆PEAK POSITION ON CCD: -100'' : 100'' AREA UNDER GAUSSIAN > 3∆AREA FLUX ERROR > 10 Creation of a database with all information The X-ray Universe 2014

QUALITY classification All useful observations 5045 (56 % of all) number of useful spectra The X-ray Universe 2014

SPATIAL EXTENT classification Distribution of the widths (FWHM) of the spatial profiles POINT-LIKE SOURCES EXTENDED SOURCES REJECTED (FITTING NOISE PEAKS) AVERAGE FWHM RGS1: 22''.2 ± 1''.6 RGS2: 20''.4 ± 1''.8 Point-like sources: 22''.2/20''.4 ± 3σ Extended sources: > 22''.2/20''.4 + 3σ The X-ray Universe 2014

PROFILE EXTENSION classification POINT-LIKE SOURCES / EXTENDED SOURCES (RGS1) ALL USEFUL SPECTRA The X-ray Universe 2014

Object types distribution TOP QUALITY POINT-LIKE SOURCES EXTENDED SOURCES MOST FREQUENT OBJECTS SEYFERT 1 GALAXIES (410) LOW MASS X-RAY BINARIES (191) BL LAC -TYPE OBJECTS (125) SUPERNOVAE REMNANT (99) CLUSTERS OF GALAXIES (233) The X-ray Universe 2014

SPECTRA The X-ray Universe 2014

Clusters of Galaxies The X-ray Universe 2014

Seyfert 1 Galaxies The X-ray Universe 2014

Seyfert 1 Galaxies High state / Low state The X-ray Universe 2014

Seyfert 2 Galaxies The X-ray Universe 2014

LINERs The X-ray Universe 2014

QSOs The X-ray Universe 2014

SNRs The X-ray Universe 2014

Emission lines Stars Star Flare Star Variable Star -of BY Dra -of RS CVn -of Orion Type -of beta Cep type -Rotationally T Tau-type Star Eclipsing binary -of Algol type -of W Uma type Spectroscopic binary Star in double system Double or multiple star High proper-motion Star Pre-main sequence Star The X-ray Universe 2014

Flare Stars The X-ray Universe 2014 The X-ray Universe 2014

T Tau-type Stars The X-ray Universe 2014

Web page Catalogue & atlas of useful RGS spectra WILL BE AVAILABLE THROUGH THE BIRD WEB PAGE http://xmm.esac.esa.int/BiRD/ ANNOUNCED IN THE XMM-NEWTON NEWSLETTER The X-ray Universe 2014

Conclusions: Atlas shows: Great potential of RGS data in archive + 5000 useful observations + 2400 very good quality → Some object classes show: similar spectral properties (continuum shape/emission lines) → While at the same time some object classes show: great diversity in spectral properties → Some object types show significant changes in: Spectral properties and flux → Some object types show: constant properties The X-ray Universe 2014 The X-ray Universe 2014

What can be done in future The interpretation of the observations in terms of physical properties and mechanisms For instance: Different abundances for different objects in same class / different classes eg. SNR with or without Fe Different ionization eg. Fe XXIV in some objects Intrinsic variability eg. Flare Stars Environment eg. Absorption due to cloud crossing the line of sight in some AGNs T h a n k y o u f o r y o u r a t t e n t i o n !