XMM-Newton Optical-UV Monitor: introduction and calibration status OM instrument and calibration
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1 XMM-Newton Optical-UV Monitor: introduction and calibration status OM instrument and calibration Antonio Talavera XMM-Newton Science Operation Centre, ESAC, ESA
2 OM: Instrument Description 30 cm Ritchey-Chretien telescope Focal ratio of f/12.7 and focal length of 3.8 m Total coverage between 170 nm and 650 nm of a 17 arcmin square field of view Filter wheel with 11 apertures: one blanked off, six broad band filters (U, B, V, UVW1, UVM2 and UVW2), one white, one magnifier and two grisms (UV and optical) Detector: micro-channel plate intensified CCD (2048 x 2048 pixels final format) OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 2
3 OM: Instrument Description Detector: micro-channel plate intensified CCD with 384 x 288 physical pixels (Active area 256x256). Amplification: 10 5 Photon events centroided to 1/8 physical pixel (2048 x 2048): 0.5 Shift and Add mechanism to compensate S/C drift or jitter Fast event timing: 500 ms in fast mode OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 3
4 OM: some examples OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 4
5 OM: some examples UV & X-ray light curves of X Spectral energy distribution of 3C273 with grisms and filters OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 5
6 OM: filters & grisms OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 6
7 OM: operational configuration with filters Two basic modes: Imaging Fast mode (< 512 pix) Default image Default image + fast mode User defined windows ( up to 5 windows, 2 in fast mode) Full-Frame Low-Resolution 1024 x pixels Full-Frame High-resolution 2048 x pixels Engineering modes (Eng 0, 1, 3, 4, 5, 6) Total number of pixels is limited Fast window: 22 x 23 Default configuration: OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 7
8 Optical Monitor: default windows OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 8
9 OM: operational configuration with grisms Single object spectroscopy: target at the boresight Field spectroscopy: all objects in the f.o.v. OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 9
10 Artefacts in OM images Straylight loops Central bright patch Gost images Streaks OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 10
11 Optical Monitor calibration: what is it? Instrumental corrections Astrometry: Geometric distortion, Boresight Photometry: Measuring the count rate of detected sources aperture PSF coincidence losses and dead time time dependent sensitivity degradation cosmetic (bad pixels) flat field (not applied in OM) All corrections are included into OM data processing through corresponding SAS CCFs Spectroscopy: Measuring the count rate of the source as a function of wavelength geometry:distortion, rotation modulo_8 wavelength flux OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 11
12 Optical Monitor calibration: what is it? PHOTOMETRY: Magnitudes: the origin m1-m2 = -2.5 log (F1/F2) F2 = Reference = Standard star = Vega m1 = -2.5 log F1 + Zero_point Zero_point = m log F2 m (OM) = -2.5 log F(OM) + Z_OM Z_OM = magnitude producing 1 count/s Standard System: UBV (Johnson) OM system (U, B & V filters) Magnitudes & colors Physical parameters, models,... Absolute Fluxes: modern photometry & spectrophotometry from magnitude to flux through Vega direct transformation: F(λ) = Κ(λ) ΟΜ (λ) Κ(λ): from spectrophotometric standard stars Κ(λ) = instrumental response (= response matrix) average K per filter Absolute fluxes Physical parameters, models,... OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 12
13 Optical Monitor calibration: what is it? SPECTROSCOPY: dispersed light wavelength scale spectral energy distribution flux scale: Inverse Sensitivity Function (ISF) ISF(λ) = Fstd (λ) / CRstd (λ) Fobs(λ) = CRobs(λ) x ISF (λ) ASTROMETRY: from detector X, Y to R.A. & Dec : S/C attitude, OM boresight, OM geometry refinement through x-correlation with catalogue (USNO) grisms: from zero order detector position to R.A. & Dec OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 13
14 OM photometry: zero points Zero points for Zero epoch The definition of the zero point (magnitude giving one count per second) can be given as: Zero_point = m_vega+2.5*alog10(countrate_vega) The count rate of Vega is obtained through simulations Zero points for OM instrumental system (at zero epoch) V B U UVW1 UVM2 UVW2 (Zero points, corrected to Johnson UBV are: ) OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 14
15 AB magnitude system for OM An input spectrum of 1 erg/s/cm2/hz gives a photon rate in each filter, n_phot. The zero points in AB system are defined as: Zero_point = * log(1./n_phot) Zero points in AB system for OM (at zero epoch) V B U UVW1 UVM2 UVW OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 15
16 OM counts to flux conversion based in white dwarfs Count rate to flux conversion (from WD's) uvw2 uvm2 uvw1 u b v e-15, 2.20e-15, 4.76e-16, 1.94e-16, 1.29e-16, 2.49e This gives erg/cm2/s/a the relative errors (stdev/mean) are : OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 16
17 OM counts to flux conversion from White Dwarfs versus Pickles and BPGS spectral libraries Pickles library BPGS library WD s 2.49E E E E E E-15 OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 17
18 OM fluxes in AB system If n_phot is the number of photons produced by 1 erg input spectrum, then 1/n_phot is the rate to flux conversion factor (in frequency space). Count rate to flux conversion in AB system (frequency) uvw2 uvm2 uvw1 u b v e e e e e e This gives erg/cm2/s/hz Note that the effective frequency of a filter can be any within the filter range since the flux is constant. Even if we are in frequency space, we can characterise the filter by its effective wavelength. OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 18
19 OM fluxes in AB system We can then convert these factors to lambda space by multiplying by (c / lambda**2 ) and we get: Count rate to flux conversion in AB system (lambda) uvw2 uvm2 uvw1 u b v e e e e e e This gives erg/cm2/s/a Not surprisingly, if we compare these last factors with the ones derived directly from WD's fluxes, we have: OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 19
20 OM Astrometry Geometric distortion distortion map derived from OM image using more than 800 stars it corrects positions to 0.7 rms error SAS provides RA & Dec for all sources detected in OM images -from X_Y, AHF (star tracker) & boresight information. Additional cross-correlation (in SAS) with USNO catalogue allows us to improve the coordinates: Using the new boresight: RMS offset from USNO < 1.5 OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 20
21 OM grisms calibration Wavelength calibration: - F-type stars:hd , HD (V & UV grisms, low & high resolution) HD 13499, HD (V & UV grisms, low resolution, across FOV) (Field stars at different positions in FOV (V & UV grisms)) - White dwarfs with Hydrogen lines (BPM 16274, GD50, ) (for V-grism) Flux calibration: - Spectrophotometric standard stars (WD): GD 153, HZ 2 Grisms distortion: - 3C273 - other science observations OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 21
22 OM grisms calibration: wavelength The wavelength scale: anchor point zero order Measuring zero-order position: it can be predicted for User Def. observing windows, (with less accuracy for full frame images), and then refined by centroiding algorithm Wavelength range: Vis-grism: A UV-grism: A (second order contamination) (the range could be extended, but not the flux calibration) Wavelength scales UV: lambda (A) = X X 2 Vis: lambda (A) = X internal error: < 7 A (UV) global shift due to zero order position: about +/- 10 A (X : pixels from zero order) OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 22
23 OM grisms data calibration: wavelength Wavelength scale variations across f.o.v.: HD offset observations and field stars in fflr science observations: Wavelength shift on right hand part of the image: up to 50 A Resolution : limited by mod_8 UV grism: better than A (from NGC 40 observations) V grism: worst than UV Mod_8 is stronger in V grism (because of higher response) OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 23
24 OM grisms data calibration: flux The Flux scale: Inverse Sensitivity Function (ISF) ISF(λ) = Fstd (λ) / CRstd (λ) Fobs(λ) = CRobs(λ) x ISF (λ) OM_GRISMCAL_0004.CCF Flux accuracy: around 10% (slightly worst at long wavelength end of V_grism) UV and V common range: excellent agreement!!! V, B, U, UVW1, UVM2, UVW2 versus Grisms: excellent agreement!!! Time sensitivity variation: < 1% p.a. OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 24
25 OM grisms& filters processed with SAS Spectrophotometric Standard Stars observed With OM OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 25
26 The Crab:OM(231, 291,344nm)versus composite X_opt_radio OM filter Count rate AB mag AB Flux (erg/cm2/s/a) UVW e-16 UVM e-16 UVW e-16 U e-15 OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 26
27 OM Calibration & SAS Continuous photometric monitoring: observations of standard WDs Time sensitivity degradation: new correction SAS repeatability & stability On-going: Visible Grism: extending calibration up to 7000 A (Halpha studies) Grisms wavelength and sensitivity variation across the f.o.v. Grisms time sensitivity degradation: determination & correction OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 27
28 OM time sensitivity degradation OM throughput Filter Current Expected in 2025 UVW UVM UVW U B V OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 28
29 Repeatability& Stability of OM photometry: BPM Average count rate Revs (26 observations): uvw2 uvm2 uvw1 u b v white (stdev %) Prediction from estimated effective area: (>> no time dependent sensitivity degradation correction for White filter) OM Instrument & Calibration A. Talavera ESAC XMM-Newton Pag. 29
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