11

John Nousek (Penn State University)Neil Gehrels (Goddard Space Flight Center)

Five Years of Science:GRBs and More!

International Workshop on Astronomical X-ray Optics - Prague, Czech Rep. – 6-9 Dec. 2009

22

Swift launch:

20 Nov 2004 !!

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5th Anniversary of Swift Conference

• Celebration of Swift held at Penn State, 18-20 Nov. 2009

• Attracted more than 150 participants – 1/3 Penn State, 1/3 US & 1/3 from ten other countries

• Discussed impact of Swift on areas of astrophysics, and planned for future developments and science direction of the Swift Observatory

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Swift has redefined the field of GRB science.

GRB backgroud

Swift comparisonsDuration

Host galaxiesDistance distributions

EnergeticsBeaming

Swift GRB Science

ARAA Annual Reviews 2009 Gehrels, Ramirez-Ruiz and Fox

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GRB PropertiesTwo types:

Short GRBs (t < 2s) Long GRBs (t > 2s)

Redshift range: 0.2 - ~2 SGRBs 0.009 - 8.2 LGRBs

Energy release in -rays: 1049-1050 ergs SGRBs 1050-1051 ergs LGRBs

Jet opening angle: ~15 deg SGRBs ~5 deg LGRBs

Both types have delayed& extended high-E emission

ARAA article

GRB 990123HST image

Fruchter et al.

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GRB Spectraprompt

afterglow withsynchrotron fit

GRB 051111

Butler et al. 2006

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VELA GRB discovery

1973

Compton / BATSE isotropy &

inhomogeneity 2 duration classes

1991

Compton / EGRET GeV extended emission

1994shortlong

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BeppoSAX afterglow & distance

1997

Fireball Model 1997

Mészáros & Rees 1997

HETE-II GRB030329 / SN2003dh

XRFs ~ 2003

BAT

XRTUVOT

3 instruments, each with:

- lightcurves - images - spectra

Rapid slewing spacecraft

Rapid telemetry to ground

.

Swift Mission

BAT Position - 2 arcmin

T<10 sec

XRT Position - 5 arcsec

T<90 sec

UVOT Position - < 1 arcsec

T<2 min

XRT

BAT

Short GRB

Short GRB

Swift Statistics475 GRB as of 1 Nov 2009

85% with X-ray detections ~60% with optical detection

155 with redshift (41 prior to Swift) 46 short GRBs localized (0 prior to Swift)

Fast Rise Exponential Decay

Swift GRB Data

UVOT image

BAT lightcurve

XRT lightcurve

GRB 091029

GRB

Swift GRB Data

BAT lightcurve

XRT lightcurve

GRB 091029flare

steep-flat-medium shape

UVOT image

GRB

1313

Shortvs

Long

short long

Time (s)

Number Gamma Rays

Time (s)

Numåber Gamma Rays

Soft

Hard

Hardness

Ratio

Duration (s)

shortlong

Kouveliotou et al. 2003

•

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GRB Spectroscopy

z Time GRB Optical Brightness

(109 years)

8.3 13.0 090423 K = 20 @ 20 min

6.7 12.8 080813 K = 19 @ 10 min 6.29 12.8 050904 J = 18 @ 3 hrs

5.6 12.6 060927 I = 16 @ 2 min

5.3 12.6 050814 K = 18 @ 23 hrs

5.11 12.5 060522 R = 21 @ 1.5 hrs

Prochaska et al. 2008

Savaglio 2006

GRB 080607

Blast from the past!GRB 090423

Lyman break redshifted from UV to IR

z = 8.29 look back time = 13.0 billion light years

GROND Greiner et al

•

Tanvir et al. 2009; Salvaterra et al. 2009

McMahon & Tanvir

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Evolution of Swift Operations – GRBs & More!• Original prime mission: 2004-2006 – Swift the GRB Explorer

• Up to Nov. 2004 – Pre-launch:– Swift primarily a GRB detection and afterglow followup mission

– Ground-breaking operations design allows immediate response to GRBs

– Automated follow-up allows introduction of new GRB without new schedule

– Targets of Opportunity limited to new non-Swift GRBs or rare events

• Expected schedule re-plans only once / month; ToO once / week

– Planning using TAKO software / five times a week• Prime mission – 2005-2006:

– Execution closely follows plans, except:• XRT TEC power supply fails, forcing operations to passively maintain XRT

below -50 C• Automated target process is great success allowing highly flexible and rapid

ToO response

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Swift Operations Currently• 1st mission extension: 2006-2008 – High-z GRBs and the GI Program

– Swift reduces time on late afterglow followup and increases effort on finding high redshift GRBs

• Swift introduces GI targets, followed by pressure for increased ToO and monitoring campaigns

– TAKO planning software modified to incorporate XRT temperature control; other ancillary software improves ACS reliability

– Improved ToO automation allows multiple ToOs in short period without new schedule (including nights and week-ends)

– Targets of Opportunity and Monitoring Campaigns occur every day

• Typical load of 4-12 ToO or Monitoring observations every day

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Supernova Studies with Swift

XRT and UVOT observations

of SNe

-66 observed to date of all types (26 Ia, 18 Ibc, 22 II)

-UV, optical & X-ray densely-sampled light curves

-Largest sample of SN light curves in the UV

-Unique UV characterizations of SN Ia's (incl UV spectra)

SN 2006bp (Type IIP)

Immler et al. 2007 Brown et al. 2008

XRT UVOT opt UVOT UV

SupernovaLightcurves

X-Ray SN Studies

Immler et al.

- XRT observations probe SNe

environments & mass-loss rates

- Signature of SN shock traveling

through dense shell

- Shells are outer H/He-rich layers

from Luminous Blue Variable phase

SN 2006jc

SN 2008bo

SN 2006bp

SN 2008D Shock Breakout

- XRT monitoring of NGC 2770 (27 Mpc)

revealed extremely luminous X-ray outburst

- EX ~ 2x1046 ergs

- No BAT, no radio late >> probably no jets

- UVOT detection of SN rising 90 min later

- SN Ib/c

- Shock breakout. May occur for all SN

Soderberg et al. 2008

9 Jan 2008

SN 2007uy

2121

- 25 novae observed

- Rise and fall of few keV

emission from shocked ejecta

- Super-Soft emission in

some from WD surface (kTBB ~ 30 eV)

- Extensive observations of

RS Oph 2006 (~400 ksec) revealed

unexpected luminous SSS state and 35

sec QPO

- Earth mass ejected at ~4000 km/s into wind of companion

Red Giant

RS Oph

Nova Studies with SwiftThermonuclear detonation of

accumulated accretion on white dwarf

1.6 kpc

2222

• BAT triggered on a stellar flare from nearby (d=5 pc) EV Lac (dM3e, Prot ~4 days)

• XRT spectra show Fe K 6.4 keV emission

first for an active dMe star

• UVOT enhancement large but unknown: instrument safed at >200,000 counts/s

• Brightest stellar flare observed

• Erad ~ 1038 erg

• EV Lac is young magnetically active

isolated star.

– Previous super-flare was from binary

RS CVn system, II Peg

Swift Trigger on Large Stellar Flare

Osten et al 2007, 2008

EV Lac25 Apr 2008

2323

Newly discovered source (Atel #1456) Known pulsar in outburst (Atel #1426)

536 sources monitored

65 detectable on a

daily basis

~60 with > 30 mcrab

outbursts

~15 mCrab sensitivity

in 1 day

http://swift.gsfc.nasa.gov/docs/swift/results/transients/

BAT Sky Monitoring

SWIFT J1816.7-1613 4U 0115+634

Krimm et al

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TOOs for Transients & GRBs

- Swift can perform rapid X-ray and optical

observations of transients

- TOO rapidly uploaded as RA & DEC. Response time

is <1 hour to 1 day

- Web page for TOO requests http://www.swift.psu.edu/too.html

- Duty scientists always on call for urgent TOOs

- New "command from home" mode for after-hour TOOs

- Expert international teams provide rapid advice* GRB follow-up (48 members)* Supernova (22 members)* CVs & novae (24 members)

* Hard X-ray survey(18 members)* AGN (4 members)

* GeV and TeV -rays(4 members)

- Daily planning telecon to decide schedules

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Swift Operations Ahead

• 2nd mission extension: 2009-2011 – Swift: the ToO Observatory– Swift executes ~70-75 separate pointings per day

• Each pointing is planned, although significant labor by human science planner to have each pointing a different target

– Under an initiative approved by 2008 Senior Review, MOC has conducted an Automation Initiative to streamline science planning

– Elements include:

• Target management database – MySQL database to automatically ingest target information from ToO requests, target lists from GI approved proposals and GRB information from GCN circulars

• More highly automated TAKO software – will allow higher automation to XRT temperature control and ACS slew behavior

– Goal is to allow faster, easier science planning, with capability to increase GI monitoring campaigns and rapid ToO response to large numbers of targets

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Conclusions

• Swift has delivered a remarkably successful science mission to date, powered by an innovative operations concept that has continued to evolve as driven by scientific interest

• The latest changes will enable an even more responsive observatory, giving more GI monitoring and ToO responsiveness

• For Senior Review 2010, How do you suggest ways to use Swift, and how is that important for astrophysics?

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Cosmic Timeline & Early Universe Probes

z=12 z=5 z=0

Hint That These Probes Work

z=6.29

GRB 050904 SDSS Quasar

z=6.28

• Swift & SDSS only probed the very near edge of reionization

• We need a statistically significant sample that probes well into the epoch of reionization– We need to find 30-50 GRBs from 5<z<12

• ~10x what Swift found (5<z<7)

– We need to find 200-400 quasars from 6<z<10• ~10x all z>6 quasars found (6<z<6.5)

We Need Higher Redshift Observations

z=12 z=5

• Current capabilities from Swift & SDSS needed to observe high redshift objects are:– Rapid localization and observations of GRBs– Rapid notifications to enable observations by other facilities– A very large field of view for finding GRBs & quasars

• BREADTH versus Depth for rare objects (Critical)

• To probe high redshift objects we need:– Greater sensitivity to high redshift bursts

• Redshifted gamma-ray photons into the X-ray

– Prompt, uniform follow-up of afterglows in the IR (Critical)– Rapid redshift determination (in minutes)– Observations above the atmosphere are essential to

eliminate terrestrial lines that confuse surveys

Current Capabilities & Needs

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The Solution: JANUS

1960 1980 2000

Testing

Support

BCD DEF

GHIJKL RST VWX XYZ TUV

Space Network

ABC

1960 1970 20201980 1990 2000 2010

Increasing Capabilities

X-Ray Flash Monitor (XRFM): Detects &

localizes high-z GRBs 1-20 keV, 4 sr field-of-

view

Near-IR Telescope (NIRT):

High-z GRB & quasar spectroscopy

0.7-1.7 μm, 1″ pos, redshifts,

0.36 degree2 field-of-view,

Spacecraft: Rapid

communication w/ ground, rapid

slewing (50°/100 sec),

stable platform

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JANUS Mission Concept – Sky Survey Mode

~400 quasars

20,000 square degreeSurvey

3333

JANUS Mission Concept – GRB Mode

~50 GRBs

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JANUS Objectives

• Determine star formation history• by using ~50 GRBs

• Explore the coevolution of galaxies & black holes • by using ~400 quasars

• Determine if dominant source of reionization