LOFT LARGE OBSERVATORY FOR X - RAY TIMING THE L ARGE O BSERVATORY F - - PowerPoint PPT Presentation

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LOFT LARGE OBSERVATORY FOR X - RAY TIMING THE L ARGE O BSERVATORY F - - PowerPoint PPT Presentation

May 12, 2023 209 likes •555 views

M ARCO F EROCI INAF , R OME ON BEHALF OF THE LOFT C ONSORTIUM LOFT LARGE OBSERVATORY FOR X - RAY TIMING THE L ARGE O BSERVATORY F OR X - RAY T IMING LOFT Consortium: national representatives: Marco Feroci INAF/IAPS-Rome, Italy Jan-Willem den

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LOFT

LARGE OBSERVATORY FOR X-RAY TIMING

MARCO FEROCI INAF , ROME

ON BEHALF OF THE LOFT CONSORTIUM

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PROBING SPACETIME AND MATTER UNDER EXTREME CONDITIONS

THE LARGE OBSERVATORY FOR X- RAY TIMING

LOFT Consortium: national representatives:

Marco Feroci INAF/IAPS-Rome, Italy Jan-Willem den Herder SRON, the Netherlands Luigi Stella INAF/OAR-Rome, Italy Michiel van der Klis

  • Univ. Amsterdam, the Netherlands

Thierry Courvousier ISDC, Switzerland Silvia Zane MSSL, United Kingdom Margarita Hernanz IEEC-CSIC, Spain Søren Brandt DTU, Copenhagen, Denmark Andrea Santangelo

  • Univ. Tuebingen, Germany

Didier Barret IRAP , T

  • ulouse, France

Renè Hudec CTU, Czech Republic Andrzej Zdziarski

  • N. Copernicus Astron. Center, Poland

Juhani Huovelin

  • Univ. of Helsinki, Finland

Paul Ray Naval Research Lab, USA Joao Braga INPE, Brazil Tad Takahashi ISAS, Japan Sudip Bhattacharyya TIFR, India LOFT Science Team composed of scientists from: Australia, Brazil, Canada, Czech Republic, Denmark, Finland, France, Germany, Greece, Ireland, Israel, Italy, Japan, the Netherlands, Poland, Spain, Sweden, Switzerland, Turkey, United Kingdom, USA

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LOFT SCIENCE

LOFT ADDRESSES THE COSMIC VISION THEME “Matter Under Extreme Conditions”

Probe gravity theory in the very strong field environment of Black Holes (“Strong Gravity”) Probe physics of hundreds of galactic and bright extragalactic cosmic sources (“Observatory Science”) Probe the state of matter at supra nuclear densities in Neutron Stars (“Dense Matter”)

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LOFT CORE SCIENCE OBECTIVES

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THE LOFT APPROACH

WHAT LOFT MUST HAVE

Exploit the Diagnostics of Spectral Variability

  • n Dynamical Timescales:

Good Energy Resolution (XMM-class) Exploit the Diagnostics of X-ray Variability

  • n Dynamical Timescales:

Large Collecting Area

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THE LOFT APPROACH

WHAT LOFT MUST HAVE

Good Energy Resolution (XMM-class) Large Collecting Area

LHC SDD Detectors Heritage Microchannel Plate Collimators

WHAT LOFT HAS!

200 eV

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RXTE 1100 eV, 0.65 m 2 XMM 130 eV, 0.085 m 2

LOFT 200 eV, 10 m 2

LOFT’S CHANGING THE GAME

LOFT UNITES SPECTROSCOPY & TIMING, AT ENORMOUS AREA

No pile-up pile-up-limited

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LOFT - LARGE AREA DETECTOR

EFFECTIVE AREA 4 m 2 @ 2 keV 10 m 2 @ 8 keV 1 m 2 @ 30 keV ENERGY RANGE 2-30 keV (30-80 keV ext.) ENERGY RESOLUTION FWHM 200 eV @ 6 keV COLLIMATED FOV 1 deg FWHM ABSOLUTE TIME ACCURACY 1 µs

2 0 0 0 x

83 µm 16 µm

1 2 5 x

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LOFT - LARGE AREA DETECTOR PERFORMANCE LAD I NSTANTANEOUS SKY VISIBILITY

75% of the sky accessibile to LAD at any time. Combination of Sky Visibility and Mission Duration ensures required number of transients

180 eV 240 eV 300 eV 340 eV

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The Key to LOFT:

  • low weight/power/volume per unit effective area
  • unprecedented large effective area
  • CCD class energy resolution
  • modularity: 126 modules made of 16 SDDs (2016 tot.)

Frame Collimators Clamps SDDs + FEEs Radiator Frame

Readout electronics (∼2.5 kg/m2) Silicon Drift Detector (∼1.3 kg/m2) MCP Collimator (∼6 kg/m2) Mechanical support, harness, interfaces LAD density ≈ 10 kg/m2 (RXTE/PCA > 100 kg/m2)

LARGE AREA DETECTOR CONCEPT

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LOFT - WIDE FIELD MONITOR

5 Units

10 Cameras FIELD OF VIEW 5.5 steradian POSITION ACCURACY (10σ) 1 arcmin ENERGY RANGE 2-50 keV ENERGY RESOLUTION 300 eV @ 6 keV COLLECTING AREA 1820 cm 2 TIME RESOLUTION 10 µs (trigger) ∼minutes (images) SENSITIVITY (5σ, GALACTIC CENTER) 270 mCrab (3s) 2.1 mCrab (1day) GROUND TRANSMISSION OF GRB COORDINATES < 30s

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LOFT - WIDE FIELD MONITOR PERFORMANCE FIELD OF VIEW EXPOSURE MAP

cm 2

Ms

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MISSION CONFIGURATION FEASIBLE MISSION IN SEVERAL CONFIGURATIONS, WITH STANDARD EQUIPMENT

Item Value

Orbit Equatorial, 550 km Launcher Soyuz (6,000 kg launch capability) Mass 4,000 kg Power 4 kW Telemetry 6.7 Gbit/orbit Ground Stations Kourou, Malindi Pointing 3-axis stabilized Mission Duration 3+2 years

South atlantic anomaly

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MISSION FEASIBILITY

Item Value

Orbit Equatorial, 550 km Launcher Soyuz Mass 4,000 kg Power 4 kW Telemetry 10 Gbit/orbit Ground Stations Kourou, Malindi Pointing 3-axis stabilized Mission Duration 3+2 years

South atlantic anomaly

ESA Review : “m ission feasible and of low technical risk and medium schedule risk for a 2022 launch date; a launch in 2 0 2 3 is seen as realistic” “The overall instrument as well as the Science Ground Segment concept is considered to be mature and well documented. The level of detail with which the instrument design is described significantly exceeds general expectations at the end of a Phase A study.” FEASIBLE MISSION IN SEVERAL CONFIGURATIONS, WITH STANDARD EQUIPMENT

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THE ESA PREFERRED LOFT CONCEPT

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PROGRAMMATICS AND SCIENCE MANAGEMENT Payload and Science Data Center provided by Institutes in ESA Member States. LOFT Science Team even wider in Europe and worldwide LOFT IS AN OPEN OBSERVATORY All LAD data open to the Community through peer-reviewed proposals. All WFM data public after validation.

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LOFT IN THE MULTI-FREQUENCY CONTEXT LOFT in the Multi-wavelength and Multi-messenger Context of Time Domain Astronomy

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LOFT Enabling Technologies

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I NSTRUMENT DEVELOPMENT IN PHASE A  Instruments

  • Detailed design (mechanical & thermal)
  • Critical technology at TRL 5 in 2014, TRL 6 in 2015 (end Phase B1)
  • Study of operational constraints & science performance

 Key T echnology

  • Detectors

 4 prototypes produced & tested  Full-scale (6-inch) LAD prototype delivered by end 2013  Radiation (soft & hard protons) and debris accelerator tests

  • ASICs

 First prototype (8 channels, analogue section) produced & tested  Second prototype (16 channels, mixed signal) delivered Jan ’14  T echnology back-up (Italian ASIC) produced and tested

  • LAD Collimator

 First prototype (pore size and thickness, half-size) produced & tested  Full scale prototype (ESA TDA) to be delivered Apr ’14

 Additional H/W development

  • WFM Mask

 Half-size prototype produced & measured

  • LAD thermal filter

 Full-scale prototype produced & tested (acoustics) in a Module frame prototype

  • MBEE, PBEE, ICU

 Electrical prototype produced & tested

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THE LARGE-AREA SILICON DRIFT DETECTOR (1991-> 2002)

20

1991

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An heritage of the Inner Tracking System of the ALICE experiment at the Large Hadron Collider (CERN):1.5 m2 of SDD detectors (approximately 300 units), operating since 2008. High TRL. Proven mass production.

LOFT TECHNOLOGY HERITAGE

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LAD Configuration:

Thickness 450 µm Monolithic Active Area 76 cm2 Drift time <5 µs Anode Pitch 970 µm Single-channel area 0.3 cm2

ALICE Large-Area Silicon Drift Detectors

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LAD – SILICON DRIFT DETECTORS SDDs Heritage of ALICE ITS (LHC) R&D IAPS, INFN-TS, FBK (Trento) for X-ray detection Advantages:

  • solid state detector
  • e- drifted and collected by small (~1 mm2) anodes → low capacitance → low series noise
  • extremely small intrinsic leakage current (< 0.05 nA/anode @ 22° C) → low parallel noise
  • 1D read-out (low power, reduced number of channels)
  • small drift time (5 µs for 35 mm drift length) → 100% CCE

Development, production & testing in Italy (INFN & INAF)

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FBK-4 (end-2013)

LAD full-scale prototype (6-inch), production batch started on late 2013. TRL 5 (TRL 6 end 2015)

ALICE (2002) FBK-1 (2010-11) FBK-2 (2011-12) FBK-3 (end-2012) Increased eff. for soft X-rays Increased thickness (450 µm) Reduced power of voltage divider Reduced surface layer thickness Larger pitch (833 µm), Larger area Design optimization Soft protons, protons, CCE LAD pitch (970 µm) WFM pitch (145 µm) Soft protons, protons, debris X-ray characterization Proton irradiation (NIEL)

SDD DEVELOPMENT (2007-

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2013, 6-inch: Leakage Current <0.09 nA cm2 !

FBK – STATE- OF-THE-ART TECHNOLOGY

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FBK – BRUNO KESSLER FOUNDATION (TRENTO, I TALY)

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Largest monolithic SDD ever built

  • Fully characterized at IAPS X-ray facility
  • Qualified for radiation damage (Del

Monte et. al, in prep.) and debris impacts

Requirement of 200 eV FWHM energy resolution (EOL) verified in LAB

~30 µm pencil beam mapping

@ IAPS facility

SDD CHARACTERIZATION @ INAF

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Variation of the CCE (11 MeV p+): PSI - Zurich (E. Del Monte et al., in prep) NIEL from 11 MeV and 50 MeV protons: PSI – Zurich (E. Del Monte et al., in prep) NIEL from soft protons (800 keV p+): Tubingen Hypervelocity impacts from debris (0.5-3 µm diameter): MPIK - Heidelberg (G. Zampa et al., in prep.)

SDD QUALIFICATION

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LOFT ASIC

  • Mixed-signal ASIC technology
  • Same ASIC design for LAD and WFM
  • Differences only related to anode pitch (capacitance, leakage current, #channels)

VEGA-1 R&D in Italy - PoliMi, Pavia Univ. (design) IAPS, IASFBo (characterization) ESA StarX32 heritage (<19 e- rms (no det), 500 μW/ch, 1024 ch)

  • CR-RC with selectable shaping time (1.6-6.6 μs)
  • C35B4C3 0.35 μm CMOS technology
  • 32 channels (200 μm x 500 μm)

LOFT baseline → Sirius ASIC: new development by Dolphin Integration

  • CR-RC2
  • 8 ch (1° prot.), 16 ch (2° prot. end-2013)
  • shaping time 1-4 μs (selectable)
  • TSMC MS/RF 0.18 μm CMOS technology
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SDD READ- OUT – THE VEGA ASIC VEGA (PoliMi, UniPv, INFN, INAF) Heritage: STARX-32

Ahangarianabhari et al. 2014

SIRIUS (IRAP, Dolphin, LAB)

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LAD - MCP COLLIMATOR MCP X-ray collimator Multi-pore, ∼mm thin sheet of lead-glass (Philips 3502, Pb 34.4%) able to absorb soft X-rays coming from outside the FoV. Holes aspect ratio 40 ÷ 200. Large-scale prototype manufactured & tested. Heritage of:

  • EXOSAT (1983-86) MEDA&GSPC detectors
  • BepiColombo Mercury Imaging X-ray Spectrometer

(MIXS) microchannel plate X-ray optics (GW Fraser et al., 2010)

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LAD COLLIMATOR 31

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ADDITIONAL H/ W DEVELOPMENT

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PERSPECTI VES

  • Very well evaluated by the ESA Technical-

Programmatic review

  • Very well received by the ESA Advisory Structure

(science)

  • preparing to run for M4 (2026)