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Deblending issues working report MontePorzio 16-04-08 CU5#DU11 Luigi INAF-OA Roma INAF - Teramo Observatory: Anna Piersimoni, Giorgia Busso INAF.

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Presentazione sul tema: "Deblending issues working report MontePorzio 16-04-08 CU5#DU11 Luigi INAF-OA Roma INAF - Teramo Observatory: Anna Piersimoni, Giorgia Busso INAF."— Transcript della presentazione:

1 Deblending issues working report MontePorzio CU5#DU11 Luigi INAF-OA Roma INAF - Teramo Observatory: Anna Piersimoni, Giorgia Busso INAF - Rome Observatory (Monte Porzio Catone): Giacinto Iannicola, Luigi Pulone, Marco Castellani ASI – ASDC (Frascati) : Licia Troisi, Roberto Buonanno, Giuliano Giuffrida Main Task Obtain a clean spectrum for every observed source, resolved in the astrometric field DU11 in CU5: Leiden (NL), Cambridge (UK), Roma,Teramo (IT)

2 Data Processing and Analysis Consortium ESA Gaia project team ESA Ground segment oversight GAIA Science TeamDPAC CU3 Core processing CU1 System architecture CU6 Spectroscopic processing CU5 Photometric processing CU2 Simulazioni CU4 Object analysis CU7 Variability analysis CU8 Astrophysical parameters

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4 Coordination Unit 5 Riduzione fotometrica e calibrazione sia in banda G che negli spettri Estrazione dei parametri delle identificazioni per ogni passaggio nel campo astrometrico Elaborazione ed accumulazione dei dati in banda G, RP, BP Identificazione stelle standard, variabili, analisi oggetti multipli Calibrazione interna ed esterna dati fotometrici Photometric science alerts

5 Gli obbiettivi di GAIA Accuratezza -4 μarcsec a V=10 10 μarcsec a V= marcsec a V=20 -Velocità radiali con accuratezza di qualche km/s complete fino a V= Survey celeste con risoluzione spaziale di 0.1 arcsec fino a V=20 - spettrofotometria multi-epoca fino a V=20 - definizione di un sistema inerziale legato ai quasar più lontani Risultati - GAIA posizionerà 300 milioni di stelle nello spazio delle fasi a 6 dimensioni e 1 miliardo di stelle nello spazio delle fasi a 5 dimensioni

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7 Formazione stellare nella Via Lattea Astrofisica stellare Struttura Galattica Fisica fondamentale Sistema di riferimento Sistema solare Pianeti extrasolari Binarie e nane brune

8 Confronto fra Hipparcos e GAIA Oggetti galassie quasar Supernovae extrag. Nuovi asteroidi binarie Nane bianche Nane brune Sistemi planetari

9 Catalogue Schedule Acceptance Technology Development Design, Build, Test Launch Observations Analysis Early Data Concept & Technology Study ESA SCI 2000(4) Re-Assessment: Ariane Soyuz To L2 Assumed start of Phase B2

10 Satellite and System Mass: 1700 kg (payload 800 kg) Power: 2000 W (payload 1200 W) ESA only mission Launch date: 2011 Lifetime: 5 years Launcher: FREGAT Orbit: L2 Ground station: Perth or Madrid Data rate: 1 Mbps

11 Il percorso ottico

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13 spettrofotometro B spettrofotometro R GAIA – Simulazione campo stellare media densità

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18 OA Teramo OA Roma, ASI-ASDC

19 OA Teramo 15.3 Anna Piersimoni, Giorgia Busso

20 OA Roma - ASDC 15.5: G. Iannicola, L. Troisi, R. Buonanno, L. Pulone, M. Castellani, G. Giuffrida

21 BPRP Gibis simulations template library obtained by Gibis 3.15 Validated! Simulator in the ranges 3500 < Teff < 20000°K, < [M/H] < 1.00

22 Teramo group Background modelling Studying relationships between AL and AC size of the source and APs Source crowding evaluation at source and transit level Create connected groups on the basis of the contamination degree Individuate isolated objects

23 BP photometer: AC width vs. G mag AC AL BP photometer: AL length vs. G mag

24 High density regions, like Galactic bulge low-extinction regions and central regions of the Large Magellanic Cloud, present a challenge both for board data-handling and for the ground-based reduction while being crucial for the Gaia science case. A recent result: expected frequency of the deblending procedure for the whole mission lifetime (~10%) taking into account the overlapping of the two field of view. Figures from Marrese & Busso 2007

25 Deblending of connected groups due to: overlapping of spectra of different sources in connected windows objects in nearby windows whose spectra extend into the program window objects for which the on-board detection software has not assigned a window barely detectable sources beyond the survey magnitude limit (20 < G < 22). Rome group

26 The numerical approach The analytical approach, has shown some limitations in reproducing high metallicity and low temperature spectra. The Rome group is now developing and testing a new deblending technique based a Marquardt-like method for non linear least square minimization. This approach is much more straightforward and makes use of the entire morphology of the spectrum simultaneously in both the Blue and Red bands. First results appear encouraging.

27 new approach template library 3500 < Teff < 20000°K, < [M/H] < 1.00 comparison between templates and input spectrum models interpolation

28 OLD ANALYTICAL vs NEW NUMERICAL APPROACH OLD NEW M/H = -5 T=8000 K Logg=4.5 Av=0.

29 test T = 9250°K, [M/H]= -4.5, -0.2, °K [M/H]T eff D T eff /T eff Simulated B Flux Fitted B flux D f B /fb Simulated R Flux Fitted R Flux D f R /f R

30 Two blended spectra in the same window T eff =20000°K, [M/H]= T eff =9000°K, [M/H]=0.00 Shift: 10 pixel

31 Recovering of blended spectra T eff T effest D T eff /T eff Simulated B Flux Fitted B flux D f B /fb Simulated R Flux Fitted R Flux D f R /f R 9000°K °K T eff =20000°K, [M/H]= T eff =9000°K, [M/H]=0.00 Shift 10 pixel

32 Central star: V=13 T=6000 [M/H]=0 Blended 1: V=14 T=10000 [M/H]=0.5 dX=15 px dY=2 px Blended 2: V=15 T=8000 [M/H]=-0.5 dX=13 dY=3

33 Next steps: Include log g into the reference theoretical template Take into account the Av Consider the paving strategy, cut windows etc. to rebuild connected and contaminated spectra


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