1. Observational Signatures of Black Hole Mergers (STSCI)
Pan-STARRS
for Observational Signatures of Black Hole Mergers (10min talk for hour discussion) - goal provide background for discussion
Subphrase - ps1 not the start by all means, many large tds (S82, INT-WFS, ROTSE/WASP/ASAS all-skys, LONEOS, QUEST, Catalina sky survey to name a few) and not the end (PTF, DES, Skymapper, LSST)
And the rise of the massive time-domain survey machines
Observational Signatures of Black Hole Mergers (STSCI)
April 1, 2009
Mark Huber (JHU)

2. Panoramic Survey Telescope And Rapid Response System
Pan-STARRS: (PS-1 prototype, ~3 yr)
Developed by UH (PI Nick Kaiser)
Construction funded by AFRL
Operations by science consortium
Concept:
Lower cost, rapid all-sky survey
Precision photometry & astrometry
Quick results, low risk
- Key project doing bh mergers? None specific, AGN kp likely interested
PI Nick Kaiser - developed by UH, hardware/infrastructure supported by USAF, operations by science consortium (lead next slide)
Prototype and provide photometric/astrometric all-sky catalog for PS4
PS concept (gene amos) -- modest telescope+large fov = low-cost, rapid all-sky survey
PS concept -- Innovative tech + excellent site = precision phot + astron
PS concept -- USAF grant + staged devel = early results+minimal risk
PS concept vs LSSTcorp -

3. PS1SC
ps1sc wiki page -
UH, IfA + National Central University, Taiwan + LCOGT - las cumbres observatory global telescope (network)
Harvard/Smithsonian Center for Astrophysics + Johns Hopkins University
Max Plank Society, Institutes in Garching and Heidelberg
Univ. of Edinburgh + Durham Univ. + Queen’s Unvi., Belfast

4. Key Projects
ISS - Populations of objects in the Inner Solar System [Jedicke]
OSS - Populations of objects in the Outer Solar System (beyond Jupiter) [Holman]
LMS - Low-Mass Stars, Brown Dwarfs, and Young Stellar Objects [Magnier, Brandner]
STS - Search for Exo-Planets by dedicated Stellar Transit Surveys [Afonso, Henning]
MW - Structure of the Milky Way and Local Group [Bell, Rix]
M31 - Dedicated Deep Survey of M31 [Seitz, Bender]
MSSP - Massive stars and supernova progenitors [Smartt, Bresolin]
CIVET - Cosmology Investigations with Variables & Explosive Transients [Tonry, Riess, Stubbs]
GAL - Galaxy Properties [Heckman, Meurer, Ferguson]
AGNHZQ - Active Galactic Nuclei and High Redshift Quasars [Chambers, Walker]
CL - Cosmological Lensing [Heavens, Kaiser, Taylor]
LSS - Large Scale Structure [Cole, Phleps, Bender]
science range from solar system to cosmology
*** note the area I’m coming from ***
Highlight civet/agn for specific interest below
CIVET+Stubbs for GW counterparts (with LIGO and/or LISA)
AGNHZQ - AGN variability, not specifically discussed but Suvi Gezari has mentioned

5. Science Analysis Servers
MOPS - Moving Object Processing System [Jedicke]
High Precision Photometry Server [Stubbs]
Photometric Classification Server [Saglia]
Transient Classification Server [Wood-Vasey]
Morphological Classification Server [Lucey]
Detection Efficiency Server [Metcalfe]
Galactic Extinction Server [Finkbeiner]
highlight 4 TCS - develop modules for classification of transients and variables
General ideas on automatec classification, feedback algorithms - bayesian methodoligies including Naïve Bayesian approach, non-parametric gaussian process regression, maybe more traditional machine learning such as neural nets and support vector machines (SVN)
See work by palomar-quest/catalina survey,

6. PS-1 Telescope and GPC1 Camera
heasley/JT talk - ~5Gbyte/min?
1.8m telescope on Haleakala (Maui) + prototype Gigpixel Camera 1 (1.4 gpixel)
40cm square focal plane with 7 sq deg field of view and 0.26” pixels
64 OTA units x 64 cells x 600 x 600 CCDs - 8x8 chips, 8x8 cells, 512x512 pixels
Order 2 TB/night, 1000 TB/yr
- PS1 will allow us to test all the technology that is being developed for Pan-STARRS, including the telescope design, the cameras and the data reduction software. PS1 will be used to make a full-sky survey
1.8m telescope on Haleakala (Maui)
1.4 gigapixel camera (GPC1)
40x40 cm focal plane
7 sq. deg. FOV, 0.26” pixels
8x8 chips, 8x8 cells per chip, 584x591 pixels

7. Orthogonal Transfer CCDs
Normal guiding (0.73”)
OT tracking (0.50”)
(nick kaiser complex 2003 talk, WP Chen)
Independently addressable cells = fast readout ~gigapixel in 2s, on-chip guiding, minimize effects of bright stars in field
tip/tilt correction on chip - compensate for image blurring

8. M31 Image/SN2008id
heasley talk - gibbous moon 1 millisec exp, M31 poster at Jan 08 AAS, M51
SN2008id discovered

9. Filter System: grizY i z r g Y
Top of atmosphere to detector - newer plot at z~1.4 and lower throughput peak~0.4
note w (g+r+I) for SS (sweet spot?) and y0 (why not - wider with more throughput) replacement - or is it Y?
Redder optical survey - y instead of u, 75 um thick devices better response towards the red
From Stefanie Phleps -
- Pan-STARRS will be a very red survey
- Good photometric redshifts only for red galaxies (LRGS -> similar to SLOAN), sig_z~<3% for LRG to z~1 (or sig_z/(1+z)?)
- For studies of galaxy properties have to combine with other surveys

10. Survey Program Summary
3p Survey (grizy, 56%)
Survey of entire visible sky (from Hawaii)
Medium Deep Survey (grizy, 25%) = MDS
10 GPC1 footprints distributed over sky
nightly depth set to reach SNIa to z>0.5
Solar System Sweet Spot Survey (i, 5%)
2 rectangles ~500 deg. at opposition region +/- 30 deg.
Stellar Transit Survey (r, 4%) = STS
3 adjacent GPC1 footprint campaign per year
Deep Survey of M31 (grizy, 2%)
Calibration Fields (grizy, 2%)
20 fields including the MDS and STS fields
MDS - y(?)
3pi, SPS - overlap will have lot of potential for transients
Also PI Discretionary time (6%)
Science motivation for survey determines cadence/depth

11. Estimated Survey Depths
3-pi
MDS
Filter
Exp.
Sat.
1 Visit
3 yr
(sec)
(mag) g 60
18.2
23.2
24.6 r 38
17.9
22.7
24.1 i
17.5
22.6
23.9 z 30
17.3
21.5
22.9 y
15.5
20.1
Exp.
1 Visit
1 yr
3 yr
(sec)
(mag)
3x240
24.8
26.7
27.3
24.4
26.3
26.9
6x240
24.3
23.7
25.6
26.2
22.3
- very approximate, still being worked out. Generally few 0.1 but definitely optimistic
For 5-sigma point source detection limits

12. Sample Survey Cadences
Visit/night
Intra-night
Inter-night
Visit/lunat.
Visit/yr
Visit/3 yr
3PI 2
TTI
4,5 d
2x3,4 band
4x5 band
12x5 band
MDS
2(gr),1(izy) 1 30
~6x30
9x30
Sweet Spot 2i
2x1 band
4x1 band
12x1 band
STS
30r
4 min
5x30
~150
M31
0-5 hr
30-60
~45x5
~675
Calib.
1,2xTTI
varies
180/band
540/band
NEED better way to illustrate…
- overlap - 30 sec cadence possible in 3pi and sweet spot
- 3pi - in a lunation have at least 3 TTI pairs for a field, and obs for 2 lunations per yr for 6 epochs
After 5 months will there be full filter set, over year will be 4 visits in each filter (2xTTI)
Separation of filter pairs goes as gri=1 or 11 month; z=6 month, y=3 or 9 month
- MD - each visible 7 MD fields will be observed each night (5 filters in 4 days) and weather=data lost
- Sweet - ~500 sq deg in each of 2 spots obs twice a night with a TTI pair in i, occurs 3 times a lunation spaced by 4 days
- STS - 1-2min exp each 3 field in r, return time 4-6 min, 3 hr long block per night? Will be calib fields as well, 120hr/yr
- M31 - setup to obs 2 in r separated up to 5 hr at 360s each, minimum of 10 consecutive weeks each year. Other filters included for 720s each night for 5 months per year.
- calib - about every hour one of the 20 cal fields will be obs for 30s, filter changes will take place if needed (ie MD)
TTI=transient time interval, visit in same filter separated by ~30min

13. Pan-STARRS(4) PS-2…3…4 4 mirror+camera design
Development ongoing
~2011(?), 10 yr survey
4 mirror+camera design
Mount type: 1 or 4?
Goal to replace UH 88” on Mauna Kea
while ps-1 is a prototype, much will be learned scientifically
Image/stats from JT 5/2008 brazil slides
PS2 first light 2009, ps4 ~2011?
replace UH 88” structure on Mauna Kea, ~10yr run and data availability dependent on operation funding sources
4 mirrors/cameras - usually pointed in same region for image combination, but option for diff filters and depending on the mount maybe point in diff direction
Surveys similar - consider so for now, just more coverage: 3pi 12 in 3 yr to 30/yr, daily MD 70 sqdeg/yr to 500/yr
pan-starrs.ifa.hawaii.edu

14. LSST (briefly) 8.4m primary (6.7m effective) Cerro Pachon, Chile
3.2 gigapixel camera, 9.6 sq. deg. FOV
~ full science operations
>20,000 sq. deg 1000x in 6 filters (ugrizy) over 10 yrs
2x15s per field, whole sky every 3-4 nights in 2 filters, ~20 day average cadence for each filter
Also specialized very deep or very fast type surveys
~ full science operations
8.4m primary (6.7 eff), 20,000 sq deg (90% of survey in deep-wide-fast), 1000x in 6 bands over 10yr, single V~24.5, stack to 27mag, whole sky every ~3-4 nights in 2 bands (~20d average cadence for each filter)
Tti pair of 15sec
Cerro Pachon in Chile (southern hemisphere, possible overlap at equator?)
National facility, “open-” source/data
wide field of view (10 square degrees), short exposures (pairs of ~15-second exposures), 3.2 gigapixel camera (~30TB/night)
6 bands (ugrizy)
10% for special surveys - very deep, very fast type survey

16. Sample Survey Cadences (partial update)
Visit/night
Intra-night
Inter-night
Visit/lunat.
Visit/yr
Visit/3 yr
3PI 2
TTI
4,5 d
2x3,4 band
4x5 band
12x5 band
MDS
2(gr),1(izy) 1 30
~6x30
18x30
Sweet Spot 2i
6x1 band
18x1 band
54x1 band
STS
30r
4 min
5x30
~150
M31
0-5 hr
30-60
~45x5
~675
Calib.
1,2xTTI
varies
180/band
540/band
NEED better way to illustrate…
- overlap - 30 sec cadence possible in 3pi and sweet spot
- 3pi - in a lunation have at least 3 TTI pairs for a field, and obs for 2 lunations per yr for 6 epochs
After 5 months will there be full filter set, over year will be 4 visits in each filter (2xTTI)
Separation of filter pairs goes as gri=1 or 11 month; z=6 month, y=3 or 9 month
- calib - about every hour one of the 20 cal fields will be obs for 30s, filter changes will take place if needed (ie MD)
- MD - each visible 7 MD fields will be observed each night (5 filters in 4 days) and weather=data lost
- Sweet - ~500 sq deg in each of 2 spots obs twice a night with a TTI pair in i, occurs 3 times a lunation spaced by 4 days
- STS - 1-2min exp each 3 field in r, return time 4-6 min, 3 hr long block per night? Will be calib fields as well, 120hr/yr
- M31 - setup to obs 2 in r separated up to 5 hr at 360s each, minimum of 10 consecutive weeks each year. Other filters included for 720s each night for 5 months per year.
TTI=transient time interval, visit in same filter separated by ~30min