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Linking Optical and Infrared Linking Optical and Infrared Observations with Gravitational Observations with Gravitational

Wave Sources. Wave Sources.

Linking Optical and Infrared Linking Optical and Infrared Observations with Gravitational Observations with Gravitational

Wave Sources. Wave Sources.

Christopher StubbsChristopher Stubbs

Department of Physics Department of Physics

DepartmeDepartment nt of Astronomyof Astronomy

Harvard UniversityHarvard Universitystubbs@physics.harvard.edustubbs@physics.harvard.edu

Christopher StubbsChristopher Stubbs

Department of Physics Department of Physics

DepartmeDepartment nt of Astronomyof Astronomy

Harvard UniversityHarvard Universitystubbs@physics.harvard.edustubbs@physics.harvard.edu

                                                 

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Some assertionsSome assertionsSome assertionsSome assertions• More celestial events have been seen at optical and IR More celestial events have been seen at optical and IR

wavelengths than have been detected in gravity waves.wavelengths than have been detected in gravity waves.

• Next generation surveys will detect essentially Next generation surveys will detect essentially allall celestially celestially variable sources, to 22nd magnitude, with variability that variable sources, to 22nd magnitude, with variability that lasts more than a few days, across entire sky*:lasts more than a few days, across entire sky*:

• Supernovae, Quasars/AGN… things that go bump in the night…

• (*except for ones hiding behind Galactic disk)

• Science would benefit from better coordination between Science would benefit from better coordination between gravity wave and optical variability community.gravity wave and optical variability community.

• More celestial events have been seen at optical and IR More celestial events have been seen at optical and IR wavelengths than have been detected in gravity waves.wavelengths than have been detected in gravity waves.

• Next generation surveys will detect essentially Next generation surveys will detect essentially allall celestially celestially variable sources, to 22nd magnitude, with variability that variable sources, to 22nd magnitude, with variability that lasts more than a few days, across entire sky*:lasts more than a few days, across entire sky*:

• Supernovae, Quasars/AGN… things that go bump in the night…

• (*except for ones hiding behind Galactic disk)

• Science would benefit from better coordination between Science would benefit from better coordination between gravity wave and optical variability community.gravity wave and optical variability community.

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Some questionsSome questionsSome questionsSome questions• What is the relationship between emission of gravity waves, What is the relationship between emission of gravity waves, and optical/infrared (OIR) radiation? and optical/infrared (OIR) radiation? • What OIR variability accompanies GW emission? What OIR variability accompanies GW emission?

• How can optical/IR observations be used in conjunction with How can optical/IR observations be used in conjunction with GW data (either detections or upper limits) to add to our GW data (either detections or upper limits) to add to our understanding? understanding?

• What is the relationship between emission of gravity waves, What is the relationship between emission of gravity waves, and optical/infrared (OIR) radiation? and optical/infrared (OIR) radiation? • What OIR variability accompanies GW emission? What OIR variability accompanies GW emission?

• How can optical/IR observations be used in conjunction with How can optical/IR observations be used in conjunction with GW data (either detections or upper limits) to add to our GW data (either detections or upper limits) to add to our understanding? understanding?

Detectable?Detectable? OIR yesOIR yes GW yesGW yes

OIR noOIR no -- ??

GW noGW no Sure, look Sure, look around…around…

--

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Linking OIR and GW dataLinking OIR and GW dataLinking OIR and GW dataLinking OIR and GW data

Optical Optical variabilityvariabilityOptical Optical variabilityvariability

Tough, due to OIR Tough, due to OIR source confusionsource confusion

We’re pretty We’re pretty good at this good at this

This link This link makes the makes the most sense most sense

to meto me

Gravity wave Gravity wave view of the skyview of the skyGravity wave Gravity wave

view of the skyview of the skyOptical view Optical view of the skyof the sky

Optical view Optical view of the skyof the sky

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(High-z Supernova Team)

Image SubtractionImage SubtractionImage SubtractionImage Subtraction

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Variability is helpful for GW optical tooVariability is helpful for GW optical tooVariability is helpful for GW optical tooVariability is helpful for GW optical too

• Pointing accuracy for eventual GW Pointing accuracy for eventual GW detections is ~ 1 degreedetections is ~ 1 degree

• Optical/IR source density is highOptical/IR source density is high

• If we limit attention to variable If we limit attention to variable sources, candidate list is 2-3 orders sources, candidate list is 2-3 orders of magnitude smaller. of magnitude smaller.

• Pointing accuracy for eventual GW Pointing accuracy for eventual GW detections is ~ 1 degreedetections is ~ 1 degree

• Optical/IR source density is highOptical/IR source density is high

• If we limit attention to variable If we limit attention to variable sources, candidate list is 2-3 orders sources, candidate list is 2-3 orders of magnitude smaller. of magnitude smaller.

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Core collapse Supernovae as Core collapse Supernovae as an illustrative examplean illustrative example

Core collapse Supernovae as Core collapse Supernovae as an illustrative examplean illustrative example

A New Mechanism for Gravitational Wave Emission in Core-Collapse A New Mechanism for Gravitational Wave Emission in Core-Collapse SupernovaeSupernovae. Ott, C. et al., PRL 96, 1102 (2006). Ott, C. et al., PRL 96, 1102 (2006)

A New Mechanism for Gravitational Wave Emission in Core-Collapse A New Mechanism for Gravitational Wave Emission in Core-Collapse SupernovaeSupernovae. Ott, C. et al., PRL 96, 1102 (2006). Ott, C. et al., PRL 96, 1102 (2006)

25 solar mass 25 solar mass progenitor progenitor

at 10 kpcat 10 kpc

SNR~100 at 10 kpcSNR~100 at 10 kpc

So LIGO might see So LIGO might see collapse of higher collapse of higher

mass objects out to mass objects out to 1 Mpc (i.e. M31)? 1 Mpc (i.e. M31)?

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A super-dupernova from a 100 A super-dupernova from a 100 solar mass progenitor?solar mass progenitor?

A super-dupernova from a 100 A super-dupernova from a 100 solar mass progenitor?solar mass progenitor?

Most luminous SN ever Most luminous SN ever seen, 75 Mpc away.seen, 75 Mpc away.

Went off during LIGO’s Went off during LIGO’s S5 run!S5 run!

Optical signature is Optical signature is hugehuge, what GW signal?, what GW signal?

We think we We think we maymay have have detected another detected another

example at z~0.8 in example at z~0.8 in ESSENCE surveyESSENCE survey

Most luminous SN ever Most luminous SN ever seen, 75 Mpc away.seen, 75 Mpc away.

Went off during LIGO’s Went off during LIGO’s S5 run!S5 run!

Optical signature is Optical signature is hugehuge, what GW signal?, what GW signal?

We think we We think we maymay have have detected another detected another

example at z~0.8 in example at z~0.8 in ESSENCE surveyESSENCE survey

N. Smith et al., astro-ph/0612617N. Smith et al., astro-ph/0612617

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PanSTARRSPanSTARRS

One estimate of optical counterparts to One estimate of optical counterparts to merging NS-NS binariesmerging NS-NS binaries

One estimate of optical counterparts to One estimate of optical counterparts to merging NS-NS binariesmerging NS-NS binaries

Sylvestre, J, ApJ 591, 1152 (2003)Sylvestre, J, ApJ 591, 1152 (2003)

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Optical/IR search optionsOptical/IR search optionsOptical/IR search optionsOptical/IR search options1.1. Look at specific galaxiesLook at specific galaxies

KAIT survey

2.2. Look at galaxy clustersLook at galaxy clusters

Mt. Stromlo cluster searchMt. Stromlo cluster search

Wise observatory searchWise observatory search

3. Look at the whole sky*3. Look at the whole sky*

Killer asteroid surveysKiller asteroid surveys: : (Spacewatch, NEAT, (Spacewatch, NEAT, LINEAR, LONEOS…)LINEAR, LONEOS…)

GRB afterglow surveys: ROTSE, WASP…GRB afterglow surveys: ROTSE, WASP…

Next generation: PanSTARRS, Skymapper, LSST…Next generation: PanSTARRS, Skymapper, LSST…

All-sky cameras, both optical and IRAll-sky cameras, both optical and IR

1.1. Look at specific galaxiesLook at specific galaxies KAIT survey

2.2. Look at galaxy clustersLook at galaxy clusters

Mt. Stromlo cluster searchMt. Stromlo cluster search

Wise observatory searchWise observatory search

3. Look at the whole sky*3. Look at the whole sky*

Killer asteroid surveysKiller asteroid surveys: : (Spacewatch, NEAT, (Spacewatch, NEAT, LINEAR, LONEOS…)LINEAR, LONEOS…)

GRB afterglow surveys: ROTSE, WASP…GRB afterglow surveys: ROTSE, WASP…

Next generation: PanSTARRS, Skymapper, LSST…Next generation: PanSTARRS, Skymapper, LSST…

All-sky cameras, both optical and IRAll-sky cameras, both optical and IR

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Survey Figure of MeritSurvey Figure of MeritSurvey Figure of MeritSurvey Figure of Merit

For a given site the system’s effectiveness scales as the A-Omega product, times For a given site the system’s effectiveness scales as the A-Omega product, times the fraction of time allotted to the survey. the fraction of time allotted to the survey.

Sensitivity to faint sources depends on aperture, not field of view. Sensitivity to faint sources depends on aperture, not field of view.

Note this simple A-Omega product neglects issues of pixel sampling, site sky Note this simple A-Omega product neglects issues of pixel sampling, site sky brightness, etc. brightness, etc.

Dynamic range per image is typically ~6 magnitudes. Can extend dynamic range Dynamic range per image is typically ~6 magnitudes. Can extend dynamic range to ~10 magnitudes using different exposure times. to ~10 magnitudes using different exposure times.

For a given site the system’s effectiveness scales as the A-Omega product, times For a given site the system’s effectiveness scales as the A-Omega product, times the fraction of time allotted to the survey. the fraction of time allotted to the survey.

Sensitivity to faint sources depends on aperture, not field of view. Sensitivity to faint sources depends on aperture, not field of view.

Note this simple A-Omega product neglects issues of pixel sampling, site sky Note this simple A-Omega product neglects issues of pixel sampling, site sky brightness, etc. brightness, etc.

Dynamic range per image is typically ~6 magnitudes. Can extend dynamic range Dynamic range per image is typically ~6 magnitudes. Can extend dynamic range to ~10 magnitudes using different exposure times. to ~10 magnitudes using different exposure times.

FOM =N / t =φ

SNR⎡

⎣⎢

⎤

⎦⎥

2AΩε

φsky(δΩ)

Source flux, Source flux, signal to noise signal to noise

System: System: Collecting Area Collecting Area Field of View Field of View

Efficiency Efficiency

Site: sky brightness, Site: sky brightness, seeing seeing

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bette

r

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Some OIR Survey SystemsSome OIR Survey SystemsSome OIR Survey SystemsSome OIR Survey SystemsSystemSystem Dia (m)Dia (m) FOV (deg)FOV (deg) A-OmegaA-Omega Mode, 60 sec 5 Mode, 60 sec 5

ConCamConCam 0.0040.004 180180 5252 All sky continuous, ~6All sky continuous, ~6

WASPWASP 0.10.1 1515 2.22.2 Triggered, ~17Triggered, ~17

ROTSE-IIIROTSE-III 0.450.45 22 0.80.8 Triggered, ~18Triggered, ~18

RaptorRaptor 0.070.07 3535 66 Triggered, ~16Triggered, ~16

ASASASAS 0.100.10 33 0.10.1 All sky, daily, ~14All sky, daily, ~14

LINEARLINEAR 1.01.0 1.41.4 1.91.9 Ecliptic, ~ 19Ecliptic, ~ 19

SDSSSDSS 2.52.5 1.5 1.5 1414 Limited survey, ~22Limited survey, ~22

VSTVST 2.62.6 11 6.86.8 Allotted time, ~22Allotted time, ~22

PS-1PS-1 1.81.8 2.62.6 2222 ““All-sky” Survey, ~22All-sky” Survey, ~22

LSSTLSST 8.58.5 3 3 650650 ““All-sky” Survey, ~24All-sky” Survey, ~24

KAIT SN surveyKAIT SN survey 0.80.8 0.10.1 0.0060.006 Close galaxies, ~19Close galaxies, ~19

Tradeoff between revisit cadence and sensitivity

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What about the Infrared?What about the Infrared?What about the Infrared?What about the Infrared?• Wavelength dependence of extinction favors an IR Wavelength dependence of extinction favors an IR

variability survey of the Galactic plane.variability survey of the Galactic plane.

• IR does better for attenuation around merging binary IR does better for attenuation around merging binary

pairs too.pairs too.

• Wavelengths beyond 2 microns are really tough from the Wavelengths beyond 2 microns are really tough from the

ground, due to blackbody emission from the atmosphere.ground, due to blackbody emission from the atmosphere.

• UKIDSS survey has recent paper on single epoch UKIDSS survey has recent paper on single epoch

Galactic plane survey, but I don’t know of any plans to do Galactic plane survey, but I don’t know of any plans to do

IR all-sky. IR all-sky.

• Absolute magnitude of type II in K band is K ~ -18.Absolute magnitude of type II in K band is K ~ -18.

• A type II behind 100 magnitudes of V band extinction A type II behind 100 magnitudes of V band extinction

would be readily detectable with ~1 m class telescope. would be readily detectable with ~1 m class telescope.

• Wavelength dependence of extinction favors an IR Wavelength dependence of extinction favors an IR

variability survey of the Galactic plane.variability survey of the Galactic plane.

• IR does better for attenuation around merging binary IR does better for attenuation around merging binary

pairs too.pairs too.

• Wavelengths beyond 2 microns are really tough from the Wavelengths beyond 2 microns are really tough from the

ground, due to blackbody emission from the atmosphere.ground, due to blackbody emission from the atmosphere.

• UKIDSS survey has recent paper on single epoch UKIDSS survey has recent paper on single epoch

Galactic plane survey, but I don’t know of any plans to do Galactic plane survey, but I don’t know of any plans to do

IR all-sky. IR all-sky.

• Absolute magnitude of type II in K band is K ~ -18.Absolute magnitude of type II in K band is K ~ -18.

• A type II behind 100 magnitudes of V band extinction A type II behind 100 magnitudes of V band extinction

would be readily detectable with ~1 m class telescope. would be readily detectable with ~1 m class telescope.

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Existing surveys already enable Existing surveys already enable “optically triggered” science“optically triggered” science

Existing surveys already enable Existing surveys already enable “optically triggered” science“optically triggered” science

Can use optical detections to run constrained “burst” Can use optical detections to run constrained “burst” search in GW data. search in GW data.

KnownKnown distances means can set SI unit limits on rate of distances means can set SI unit limits on rate of change of quadrupole moments. change of quadrupole moments.

Great recent example of looking for GW signature from Great recent example of looking for GW signature from external trigger is: LIGO team & Hurley, external trigger is: LIGO team & Hurley, Implications for Implications for the Origin of GRB 070201 from LIGO Observations, the Origin of GRB 070201 from LIGO Observations, ((arXiv:0711.1163)arXiv:0711.1163)

Can use optical detections to run constrained “burst” Can use optical detections to run constrained “burst” search in GW data. search in GW data.

KnownKnown distances means can set SI unit limits on rate of distances means can set SI unit limits on rate of change of quadrupole moments. change of quadrupole moments.

Great recent example of looking for GW signature from Great recent example of looking for GW signature from external trigger is: LIGO team & Hurley, external trigger is: LIGO team & Hurley, Implications for Implications for the Origin of GRB 070201 from LIGO Observations, the Origin of GRB 070201 from LIGO Observations, ((arXiv:0711.1163)arXiv:0711.1163)

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SNe that coincided with S5SNe that coincided with S5SNe that coincided with S5SNe that coincided with S5

QuickTime™ and aTIFF (LZW) decompressor

are needed to see this picture.

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Some are of potential interest…Some are of potential interest…Some are of potential interest…Some are of potential interest…

762 supernovae 762 supernovae during S5during S5

762 supernovae 762 supernovae during S5during S5

411 core collapse 411 core collapse (spectral confirm.)(spectral confirm.)

411 core collapse 411 core collapse (spectral confirm.)(spectral confirm.)

89 in named 89 in named galaxiesgalaxies

89 in named 89 in named galaxiesgalaxies

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Went to “virtual observatory” Went to “virtual observatory” Went to “virtual observatory” Went to “virtual observatory”

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QuickTime™ and aTIFF (LZW) decompressor

are needed to see this picture.

Closest FewClosest FewClosest FewClosest Few

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One potential search schemeOne potential search schemeOne potential search schemeOne potential search schemeLocations known to subarcsec accuracy, plus redshifts. Locations known to subarcsec accuracy, plus redshifts.

This implies arrival time This implies arrival time differencesdifferences at different GW antennas are at different GW antennas are known to dt ~ dknown to dt ~ d * L/c ~ (5E-6)*(1000 km)/c ~ tens of nanosec. * L/c ~ (5E-6)*(1000 km)/c ~ tens of nanosec. Delay between optical peak flux and GW transient is unknown. Delay between optical peak flux and GW transient is unknown.

So do fixed-delay autocorrelation analysis, sliding over plausible So do fixed-delay autocorrelation analysis, sliding over plausible window in arrival time. This amounts to blending the burst window in arrival time. This amounts to blending the burst detection algorithms with known-source analysis. detection algorithms with known-source analysis.

Could also imagine a stacking scheme, that averages over Could also imagine a stacking scheme, that averages over multiple optical trigger events (Bence Kocsis).multiple optical trigger events (Bence Kocsis).

Locations known to subarcsec accuracy, plus redshifts. Locations known to subarcsec accuracy, plus redshifts.

This implies arrival time This implies arrival time differencesdifferences at different GW antennas are at different GW antennas are known to dt ~ dknown to dt ~ d * L/c ~ (5E-6)*(1000 km)/c ~ tens of nanosec. * L/c ~ (5E-6)*(1000 km)/c ~ tens of nanosec. Delay between optical peak flux and GW transient is unknown. Delay between optical peak flux and GW transient is unknown.

So do fixed-delay autocorrelation analysis, sliding over plausible So do fixed-delay autocorrelation analysis, sliding over plausible window in arrival time. This amounts to blending the burst window in arrival time. This amounts to blending the burst detection algorithms with known-source analysis. detection algorithms with known-source analysis.

Could also imagine a stacking scheme, that averages over Could also imagine a stacking scheme, that averages over multiple optical trigger events (Bence Kocsis).multiple optical trigger events (Bence Kocsis).

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Imminent (~12 mo)Imminent (~12 mo) Imminent (~12 mo)Imminent (~12 mo) • PanSTARRS 1PanSTARRS 1

• 1.8 m aperture• 7 square degree field• 1.4 Gpix imager• Deep depletion detectors• Latitude +20

• SkymapperSkymapper• 1.35 m aperture• 5.7 sq degrees• Bands optimized for stellar astronomy• Latitude 30

• PanSTARRS 1PanSTARRS 1• 1.8 m aperture• 7 square degree field• 1.4 Gpix imager• Deep depletion detectors• Latitude +20

• SkymapperSkymapper• 1.35 m aperture• 5.7 sq degrees• Bands optimized for stellar astronomy• Latitude 30

PS 1 on HaleakalaPS 1 on Haleakala

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PanSTARRS first PanSTARRS first light image of light image of

M31, Andromeda M31, Andromeda galaxy.galaxy.

PS-1 should PS-1 should detect anything of detect anything of interest in M31, in interest in M31, in

its microlensing its microlensing survey data set, survey data set,

from 2009-2011. from 2009-2011.

PanSTARRS first PanSTARRS first light image of light image of

M31, Andromeda M31, Andromeda galaxy.galaxy.

PS-1 should PS-1 should detect anything of detect anything of interest in M31, in interest in M31, in

its microlensing its microlensing survey data set, survey data set,

from 2009-2011. from 2009-2011.

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PanSTARRS-1: PanSTARRS-1: 200 supernovae/month!200 supernovae/month!PanSTARRS-1: PanSTARRS-1: 200 supernovae/month!200 supernovae/month!1.8m telescope, 7 square degree FOV1.8m telescope, 7 square degree FOV

Telescope now in shakedownTelescope now in shakedown

1.4 Gpix camera, first light in Sept 2007 1.4 Gpix camera, first light in Sept 2007

Image processing pipeline runs end-to-endImage processing pipeline runs end-to-end

Operations likely to begin late 2008Operations likely to begin late 2008

Expect ~ 1 orphan afterglow visible at any timeExpect ~ 1 orphan afterglow visible at any time

1.8m telescope, 7 square degree FOV1.8m telescope, 7 square degree FOV

Telescope now in shakedownTelescope now in shakedown

1.4 Gpix camera, first light in Sept 2007 1.4 Gpix camera, first light in Sept 2007

Image processing pipeline runs end-to-endImage processing pipeline runs end-to-end

Operations likely to begin late 2008Operations likely to begin late 2008

Expect ~ 1 orphan afterglow visible at any timeExpect ~ 1 orphan afterglow visible at any time

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• Dark Energy SurveyDark Energy Survey• Equip CTIO 4m with 3 sq deg camera• 1/3 of the time, 5 year survey• Cluster photo-z’s, SNe, Weak Lensing, LSS

• PanSTARRS 4PanSTARRS 4• Four 1.8m telescopes, PS-1 is prototype

• Large Synoptic Survey TelescopeLarge Synoptic Survey Telescope• 8.4m aperture• 9.6 sq degree field

• Dark Energy SurveyDark Energy Survey• Equip CTIO 4m with 3 sq deg camera• 1/3 of the time, 5 year survey• Cluster photo-z’s, SNe, Weak Lensing, LSS

• PanSTARRS 4PanSTARRS 4• Four 1.8m telescopes, PS-1 is prototype

• Large Synoptic Survey TelescopeLarge Synoptic Survey Telescope• 8.4m aperture• 9.6 sq degree field

In the Planning/Design phaseIn the Planning/Design phaseIn the Planning/Design phaseIn the Planning/Design phase

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Large Synoptic Survey TelescopeLarge Synoptic Survey TelescopeLarge Synoptic Survey TelescopeLarge Synoptic Survey TelescopeHighly ranked in Decadal SurveyHighly ranked in Decadal Survey

Optimized for time domainOptimized for time domain

scan modescan mode

deep modedeep mode

10 square degree field10 square degree field

6.5m effective aperture6.5m effective aperture

24th mag in 20 sec24th mag in 20 sec

>20 Tbyte/night>20 Tbyte/night

Real-time analysisReal-time analysis

Simultaneous multiple science goalsSimultaneous multiple science goals

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LSST Merges 3 Enabling Technologies LSST Merges 3 Enabling Technologies LSST Merges 3 Enabling Technologies LSST Merges 3 Enabling Technologies

• Large Aperture OpticsLarge Aperture Optics

• Computing and Data Storage Computing and Data Storage

• High Efficiency DetectorsHigh Efficiency Detectors

• Large Aperture OpticsLarge Aperture Optics

• Computing and Data Storage Computing and Data Storage

• High Efficiency DetectorsHigh Efficiency Detectors

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One blind spot = The Milky WayOne blind spot = The Milky WayOne blind spot = The Milky WayOne blind spot = The Milky WaySpans large solid angle on the sky, Galactic center is at 18 Spans large solid angle on the sky, Galactic center is at 18 degrees South.degrees South.

LSST might not even observe at low galactic latitude, due to LSST might not even observe at low galactic latitude, due to high stellar densities (!).high stellar densities (!).

Disk of Galaxy has high extinction in the optical due to “dust”. Disk of Galaxy has high extinction in the optical due to “dust”. This produces the “zone of avoidance” in galaxy catalogs, etc.This produces the “zone of avoidance” in galaxy catalogs, etc.

But the MW sources we’re seeking (from the GW context) are But the MW sources we’re seeking (from the GW context) are going to be really bright transients in the optical/IR. going to be really bright transients in the optical/IR.

These considerations motivate an on going modest-aperture These considerations motivate an on going modest-aperture wide angle IR survey that includes the plane of MW. wide angle IR survey that includes the plane of MW.

Spans large solid angle on the sky, Galactic center is at 18 Spans large solid angle on the sky, Galactic center is at 18 degrees South.degrees South.

LSST might not even observe at low galactic latitude, due to LSST might not even observe at low galactic latitude, due to high stellar densities (!).high stellar densities (!).

Disk of Galaxy has high extinction in the optical due to “dust”. Disk of Galaxy has high extinction in the optical due to “dust”. This produces the “zone of avoidance” in galaxy catalogs, etc.This produces the “zone of avoidance” in galaxy catalogs, etc.

But the MW sources we’re seeking (from the GW context) are But the MW sources we’re seeking (from the GW context) are going to be really bright transients in the optical/IR. going to be really bright transients in the optical/IR.

These considerations motivate an on going modest-aperture These considerations motivate an on going modest-aperture wide angle IR survey that includes the plane of MW. wide angle IR survey that includes the plane of MW.

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Another blind spot: Really bright things! Another blind spot: Really bright things! Another blind spot: Really bright things! Another blind spot: Really bright things!

A type II SN in M31 would peak at about m = A type II SN in M31 would peak at about m = 19 19 24.3 = 5th 24.3 = 5th magnitude. magnitude.

This is really bright! LSST will This is really bright! LSST will saturatesaturate on objects 10 on objects 1055 X fainter! X fainter!

At present we do not have a well-thought-out strategy to hand off At present we do not have a well-thought-out strategy to hand off objects across the system of telescopes of different apertures, as objects across the system of telescopes of different apertures, as they rise and fall in brightness. There are calibration challenges they rise and fall in brightness. There are calibration challenges due to mis-matched filters and detector efficiencies vs. due to mis-matched filters and detector efficiencies vs. wavelength. wavelength.

A type II SN in M31 would peak at about m = A type II SN in M31 would peak at about m = 19 19 24.3 = 5th 24.3 = 5th magnitude. magnitude.

This is really bright! LSST will This is really bright! LSST will saturatesaturate on objects 10 on objects 1055 X fainter! X fainter!

At present we do not have a well-thought-out strategy to hand off At present we do not have a well-thought-out strategy to hand off objects across the system of telescopes of different apertures, as objects across the system of telescopes of different apertures, as they rise and fall in brightness. There are calibration challenges they rise and fall in brightness. There are calibration challenges due to mis-matched filters and detector efficiencies vs. due to mis-matched filters and detector efficiencies vs. wavelength. wavelength.

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All-sky cameras exist alreadyAll-sky cameras exist alreadyAll-sky cameras exist alreadyAll-sky cameras exist already

ConCam project ConCam project

R. Nemiroff, MTUR. Nemiroff, MTU

http://nightskylive.net/index.phphttp://nightskylive.net/index.php

Is anyone mining this open-accessIs anyone mining this open-access data set to search for bright (nearby) data set to search for bright (nearby)

transients?transients?

ConCam project ConCam project

R. Nemiroff, MTUR. Nemiroff, MTU

http://nightskylive.net/index.phphttp://nightskylive.net/index.php

Is anyone mining this open-accessIs anyone mining this open-access data set to search for bright (nearby) data set to search for bright (nearby)

transients?transients?

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Some OpportunitiesSome OpportunitiesSome OpportunitiesSome Opportunities• Undertake “pointed” GW analysis to look for transient signals Undertake “pointed” GW analysis to look for transient signals associated with known SNe. Maybe even co-add?associated with known SNe. Maybe even co-add?

• Ensure optical coverage of all local group galaxies, especially Ensure optical coverage of all local group galaxies, especially our own, to detect bright transients. Although rare, let’s not our own, to detect bright transients. Although rare, let’s not miss it!miss it! • Undertake frame subtraction processing of ConCam data set, Undertake frame subtraction processing of ConCam data set, and other similar all-sky imagers, taking care to not suppress and other similar all-sky imagers, taking care to not suppress saturation-level sources. saturation-level sources.

• Consider in more detail the likely OIR signatures of inspiraling Consider in more detail the likely OIR signatures of inspiraling GW sources, and coordinate with large-aperture surveys GW sources, and coordinate with large-aperture surveys (PanSTARRS, LSST…). (PanSTARRS, LSST…).

• Undertake “pointed” GW analysis to look for transient signals Undertake “pointed” GW analysis to look for transient signals associated with known SNe. Maybe even co-add?associated with known SNe. Maybe even co-add?

• Ensure optical coverage of all local group galaxies, especially Ensure optical coverage of all local group galaxies, especially our own, to detect bright transients. Although rare, let’s not our own, to detect bright transients. Although rare, let’s not miss it!miss it! • Undertake frame subtraction processing of ConCam data set, Undertake frame subtraction processing of ConCam data set, and other similar all-sky imagers, taking care to not suppress and other similar all-sky imagers, taking care to not suppress saturation-level sources. saturation-level sources.

• Consider in more detail the likely OIR signatures of inspiraling Consider in more detail the likely OIR signatures of inspiraling GW sources, and coordinate with large-aperture surveys GW sources, and coordinate with large-aperture surveys (PanSTARRS, LSST…). (PanSTARRS, LSST…).

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Some Open QuestionsSome Open QuestionsSome Open QuestionsSome Open QuestionsWon’t most detectable GW sources have Won’t most detectable GW sources have accompanying OIR variability? How detectable is this? accompanying OIR variability? How detectable is this?

Is there merit in establishing coordination and data Is there merit in establishing coordination and data reduction pipeline for existing all-sky survey programs?reduction pipeline for existing all-sky survey programs?

Drawing a lesson from GRB science, where xray and Drawing a lesson from GRB science, where xray and optical data did better jointly than separately, how can optical data did better jointly than separately, how can we best merge xray, OIR, neutrino and gravity wave we best merge xray, OIR, neutrino and gravity wave data? data?

Won’t most detectable GW sources have Won’t most detectable GW sources have accompanying OIR variability? How detectable is this? accompanying OIR variability? How detectable is this?

Is there merit in establishing coordination and data Is there merit in establishing coordination and data reduction pipeline for existing all-sky survey programs?reduction pipeline for existing all-sky survey programs?

Drawing a lesson from GRB science, where xray and Drawing a lesson from GRB science, where xray and optical data did better jointly than separately, how can optical data did better jointly than separately, how can we best merge xray, OIR, neutrino and gravity wave we best merge xray, OIR, neutrino and gravity wave data? data?

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SummarySummarySummarySummaryOptically triggered GW analysis will deliver real science from Optically triggered GW analysis will deliver real science from upper limits, and eventually linking detections to optical upper limits, and eventually linking detections to optical counterparts will aid interpretation:counterparts will aid interpretation:

Characterize astrophysics of sourcesCharacterize astrophysics of sourcesIndependent determination of both redshift and distanceIndependent determination of both redshift and distance

Optical all-sky surveys (down to faint flux levels) will soon be in Optical all-sky surveys (down to faint flux levels) will soon be in operation. We should be able to correlate optical variability with operation. We should be able to correlate optical variability with inspiraling compact object pairs, assuming OIR emission, even inspiraling compact object pairs, assuming OIR emission, even if variability is subtle. if variability is subtle.

We are less well instrumented/organized for early detection of We are less well instrumented/organized for early detection of bright SNe in the local group of galaxies. SN 1987A in LMC bright SNe in the local group of galaxies. SN 1987A in LMC was found by eye! Two decades later, this would likely again be was found by eye! Two decades later, this would likely again be the case. the case.

Optically triggered GW analysis will deliver real science from Optically triggered GW analysis will deliver real science from upper limits, and eventually linking detections to optical upper limits, and eventually linking detections to optical counterparts will aid interpretation:counterparts will aid interpretation:

Characterize astrophysics of sourcesCharacterize astrophysics of sourcesIndependent determination of both redshift and distanceIndependent determination of both redshift and distance

Optical all-sky surveys (down to faint flux levels) will soon be in Optical all-sky surveys (down to faint flux levels) will soon be in operation. We should be able to correlate optical variability with operation. We should be able to correlate optical variability with inspiraling compact object pairs, assuming OIR emission, even inspiraling compact object pairs, assuming OIR emission, even if variability is subtle. if variability is subtle.

We are less well instrumented/organized for early detection of We are less well instrumented/organized for early detection of bright SNe in the local group of galaxies. SN 1987A in LMC bright SNe in the local group of galaxies. SN 1987A in LMC was found by eye! Two decades later, this would likely again be was found by eye! Two decades later, this would likely again be the case. the case.