Save the sky adventures in sky monitoring
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Save the Sky: Adventures in Sky Monitoring. Robert J. Nemiroff. Who am I ?. Most cited science papers: GRBs: time dilation, cosmology, lens searches Microlensing: finite source size effects, AGN BLR probe Favorite science papers :

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Save the sky adventures in sky monitoring

Save the Sky: Adventures in Sky Monitoring

Robert J. Nemiroff


Who am i

Who am I?

  • Most cited science papers:

    • GRBs: time dilation, cosmology, lens searches

    • Microlensing: finite source size effects, AGN BLR probe

  • Favorite science papers:

    • On the Probability of Detection of a Single Gravitational Lens (1989)

    • Visual Distortions Near a Black Hole and Neutron Star (1993)

    • Toward a Continuous Record of the Sky (1999)

    • Tile or Stare? Cadence and Sky-monitoring Observing Strategies That Maximize the Number of Discovered Transients (2003)


Who am i know your visitors

Who am I?(Know your visitors)

  • Web:

    • Black hole movies at: http://antwrp.gsfc.nasa.gov/htmltest/rjn_bht.html

      GR correct! (Could make another IAS talk)

    • Astronomy Picture of the Day at:

      http://apod.nasa.gov/

      NASA’s top-ranked site!


Save the sky

Save the Sky

  • What happened in the sky last night?

    • Supernova? Nova? Eta Carina flare?

      GRB afterglow? Undocumented flash? Flurry of sporadic meteors?

    • Clouds obscure your remote observing?

    • Cirrus affect data on Jan 22 at KPNO?

    • Are clouds rolling in just now?

    • Is last night’s sky gone forever?


Save the sky1

Save the Sky

  • Popular Name:

    The Night Sky Live Project

  • Web address: http://concam.net

  • Deploys CONtinuous CAMeras (CONCAMs)


Concam objectives

CONCAM: Objectives

  • Primary Science

    • Unprecedented temporal monitoring for GRB OTs, meteors, variable stars, comets, novae, supernovae

  • Support Science

    • Unprecedented ability to act as instantaneous cloud monitors, archival cloud monitors, generate all-sky transparency maps, all-sky emissivity maps

  • Education / Outreach

    • Unprecedented ability to show your class last night’s (real) sky, archival skies, monitor meteor showers in real time, show educational sky movies, run educational modules


Concam locations

CONCAM Locations


Save the sky 4 concam locations

Save the Sky: 4 CONCAM locations

Kitt Peak

Mt. Wilson

Mauna Kea

Wise Obs.


Concam hardware

CONCAM: Hardware

  • CONCAMs are essentially fisheye lenses attached to CCDs run by a PC computer and connected to the internet. CONCAMs do not move - they are completely passive.

    • Most simply put: light comes in the top, electricity comes in the bottom, and data flow out the bottom.

  • In building CONCAMs, we have three montras:

    • “If it moves, it breaks.”

    • “The lens IS the dome.”

    • “Don’t spend 90% of your time trying to get 10% more images.”


Concam data

CONCAM: Data

  • All recent images are available through http://concam.net

  • All data are free and public domain.

  • All FITS and JPG data are archived to DVDs (previously CDs).

  • Each CONCAM node generates about 500Mb of raw image data per night.

  • Higher level data products (e.g. photometry) are now being generated in real time for some CONCAMs.


Concam scientific milestones

CONCAM Scientific Milestones

  • First CCD device to image the position of a gamma-ray burst during the time of the gamma-ray burst trigger (#1: GRB 001005)

  • Most complete, global, and uniform coverage of a meteor storm: the 2001 Leonids

  • Most complete light curves for hundreds of bright variable stars starting from May 2000, when the first CONCAM was deployed on Kitt Peak.

  • First devices to give real-time optical ground truth for the whole sky in support of major astronomical telescopes, including Gemini North, Keck, Subaru, IRTF, SpaceWatch, Wise, ING 4-m, Mayall 4-M, SARA, and WIYN.

  • In May 2003, fisheye night sky webcams now image most of the night sky, most of the time. For example, were SN 1987A to go off tomorrow, there would be a good chance that a CONCAM saw it.


Tile or stare a sky monitor s classic conundrum

Tile or Stare?A sky monitor’s classic conundrum

  • Sky monitoring increasing

    • Current Projects (see BP webpage: abridged, expanded)

    • CONCAM R. J. Nemiroff

    • KAITA. Filippenko

    • LINEARLINEAR team

    • LONEOS T. Bowell

    • LOTISH. S. Park

    • MEGAA. Crotts

    • NEATE. Helin

    • RAPTORW. T. Vestrand

    • ROTSEC. Ackerloff

    • SpacewatchR. S. McMillan

    • STARET. M. Brown

    • SuperMACHOC. Stubbs

    • TAOSC. Alcock

    • YSTARY. I. Byun


Tile or stare

Tile or Stare?

  • Likely future sky monitoring projects

    include (much abridged):

  • Pan-STARRSN. Kaiser

  • LSSTA. Tyson

  • GLASTP. F. Michelson


Tile or stare assumptions

Tile or Stare?: Assumptions

Generic case considered here:

  • Transients are discovered and confirmed on a time-contiguous series of exposures

  • Sky is isotropic

  • Effective apparent brightness distribution of transients N(l) is already known

  • Once discovered, transients are handed off to a separate follow-up telescope

    “Tile or Stare” & tiling cadence determination important for:

  • microlensing, GRB OTs, supernovae, planet detection, binary star eclipses, stellar flares, blazar flares, QSO flares, Near Earth Objects, comets, meteors & more ...


Tile or stare the two key power indices

Tile or Stare?The Two Key Power Indices: ,

  • Variables:

    • N: effective apparent cumulative brightness distribution of transients

    • ldim: apparent luminosity at obs. limit

    • te: exposure time

  • At the observation limit, quantify:

    • N  ldim(low background:   -1)

    • ldim te(high background :   -1/2)

  • N  te


Tile or stare a mathematical optimization

Tile or Stare?: A Mathematical Optimization

  • Find N(l) from existing observations (l: apparent brightness)

  • Find l(te) from detector, noise, and backgrounds (te: exposure time)

  • Compute N(te) -- might be conveniently parameterized in terms of power-law indices  & 

  • Estimate total time of campaign: tc (exact value usually not important)

  • Find grand total expected transients during campaign: Ng

  • Write Ng is terms of treturn, the time it takes for a survey to return to a given field (i.e. cadence). Read, down and slew times enter here.

  • Compute dNg/dtreturn, find solutions to dNg/dtreturn=0.

  • Find treturn that best maximizes Ng.


Save the sky cadence

Save the Sky: Cadence


Tile or stare cadence

Tile or Stare: Cadence


Tile or stare cadence1

Tile or Stare: Cadence


Tile or stare decision summary

Tile or Stare? Decision Summary

  • If, during exposure, the rate that transients come over the limiting magnitude horizon is increasing fast enough (  > 1), then stare should be preferred.

  • If, on the other hand, the rate that transients come over the limiting magnitude horizon is not increasing fast enough (  < 1), then tile should be preferred.

  • Usually the best tiling cadence is the duration of the transient, since a faster tiling cadence will waste effort on transients that have been previously discovered, while a slower tiling cadence will miss transients occurring in other fields.

  • If, however, the duration of the transient is comparable to the cumulative read-out and/or slew times during a sky-tiling, then a mathematical maximization as described in the preprint will find the most productive cadence.


Tile or stare supermacho

Tile or Stare? SuperMACHO

  • Objective: maximize microlensing transients discovered

  • LMC N(l) has  < 1: tile beats stare for identical fields

    • what cadence?

  • LMC not isotropic: fields with highest N(ldim) preferred

    • N(l) may change with seeing or be better determined with time

    • Therefore, choosing the next field to observe is very complicated -- not unlike a chess game. Optimization might involve real-time Monte-Carlo simulations.

  • Field return rate still attracted toward transient “duration of interest”

    • faster cadence inefficiently re-discovers known microlenses (competes with field richness at ldim)

    • “duration of interest” may be the microlens rise time: ~ two weeks, although microlens rise times have wide variety of durations


Tile or stare lsst

Tile or Stare?: LSST

  • Objective (example): maximizing Type IA supernovae discovered

  • Sky essentially isotropic (out of Galactic plane)

  • N(l):  > 1 for I < 24: stare preferred

    • effectively creates a minimum observation time per field

  • N(l):  < 1 for I < 24: tile preferred

    • what cadence?

  • Return time (cadence) optimized at the “duration of interest”

    • faster cadence inefficiently re-discovers known supernovae

    • slower cadence inefficiently misses supernovae in neglected fields

    • “duration of interest” could be rise time of SNe: ~ 15 days (1+z)

  • Different cadences will optimize discovery rates for different transients

    • might have Guest Investigators (GIs) program where GIs change filters and cadence to optimize discovery rate of GI-preferred transients


Tile or stare glast

Tile or Stare?: GLAST

  • Objective: maximize blazars (quiescent phase) discovered

  • GLAST’s survey mode constrains it to point away from the Earth, but rock at some cadence between the N&S Celestial Poles.

  • N(l) away from Galactic Plane:  > 1: stare

    • stare = GLAST Deep Field (GDF); should maximize detections

    • stare only possible at NCP, SCP or during pointing mode

    • GDF exposures should end if/when faint blazars saturate ( drops below unity)

  • N(1) in Galactic Plane:  < 1: tile

    • GDF strategy inefficient in Galactic Plane

    • quiescent nature allows co-adding at any time, cadence unimportant

  • , , GDF existence, GDF location are energy dependant.


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