First results from The Palomar Transient Factory Eran Ofek Einstein fellow CALTECH.

First results fromThe

Palomar Transient Factory

Eran OfekEinstein fellow

CALTECH

Talk Layout

PTF goals

System overview

Capabilities and products

What have we found so far?

Next Generation Transients Factory

PTF collaborationPI: S. R. Kulkarni

Caltech, LCOGT, Berkeley, LBL, IPAC, Columbia, Oxford, Weizmann

PTF goals

To study the transient and variable sky

Core collapse SNe

Calibrating SN Ia for cosmology

Explore new regions of transients parameter space

Stellar variability: RR Lyr, AM CVn,…

Solar system: Asteroid rotations

Law et al., Rau et al.

PTF system overview

48” Oschin Schmidt camera (Palomar obs.)

7.2 deg2 FOV (92 Mpix)

Scale: 1”/pix, lim. mag ~21

Robotic telescope & scheduler Full automatic operation Auto. Selection of science targets

PTF system overview

60s exposure + 35s readout ~510,000 deg2 yr-1

Filters: g, R, H+

Real time imageSubtraction andTransientclassification

PTF system overviewReal time transient classification

Galaxy zoo transient

PTF observing strategy Observing strategy

40% : 3-day cadence

40% : 1-day cadence

10% : All sky H survey

10% : Monitoring of star formation regions

PTF followup

What did we observe so far?

Log 1

0(N

imag

es)

Abs. photometry

Abs. photometry calibration good to 2-3%

Using SDSS starsas standard stars tocalibrate fields outsideSDSS footprint(photometric nights)

CCD 4

Relative photometry

Relative photometry ~3-5mmag

Deep coadd

Deep sky:~10 images lim. mag. ~22.5~100 images lim. mag. ~24

Data ReleaseFirst public data release: 2011

GalacticWhat have we found?

Galactic: 51 dwarf novae

3 AM CVn

Planet candidates around M-dwarfs

PTF 10nvg: enhanced accretion and outflow in Class-I protostar

New FU Ori star

Levitan et al., in prep.

Law et al., in prep.

Covey et al., 1011.2565

Miller et al., 1011.2063

AM CVnPrimary background noise for LISA

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FU Ori and otherPTF10qpf: new FU Ori star

Miller et al., 1011.2063

Planets around M-dwarfsOnly 16 planetary systems detected around M-dwarfs

Possible to find planets in the habitable zone…

Calibrating the mass-radius relation of M-dwarfs

Law et al., in prep.

Planets around M-dwarfsSome eclipsing M-dwarfs we found…

Planets around M-dwarfs

Consistent with secondary radius ~ 1.5-2.0 RJ

Law

et

al.,

in p

rep.

Planets around M-dwarfsLa

w e

t al.,

in p

rep.

Asteroids rotationPoolis

hok

et

al.,

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.

ExtragalacticWhat have we found?

Since March 2009: >5,000 transient candidates 1036 spectroscopically confirmed SNe 692 Ia 49 Ibc 257 II~3% of these “SNe” are weird and hard to classify into existing scheme:e.g., faint and fast, Ca rich, luminous, etc. Kasliwal et al., 1005.1455

Kasliwal et al., ApJ 723, 98

HST UV spectra of Ia SNePTF Can find SN Ia early PI: R. Ellis

HST UV spectra of Ia SNeThe first dozen…Cooke et al., 1010.2211

HST UV spectra of Ia SNeCooke et al., 1010.2211

The mean UV spectrum of the z~0 and z~0.5 agree, but somedifferences inmetallicabsorptions

The hosts of CC SNeArcavi et al., ApJ 721, 777

MR<-18 MR>-18

Ic-BL and IIb are more common in dwarf hosts,Stripped CC (Ic) are not seen in dwarf hosts.

Probably because in lower metallicity hosts,Metallicity-driven mass loss is reduced.

The SN2005E family

>23 kpc from NGC 1032No host: MR>-7Spec: He burning products Ca reach

Possibilities:Acc. Induced Collapse.Ia

May solve puzzles:

44Ca in Solar System44Ti->44Ca via b decayPositrons annihilationin Galactic bulge

Perets et al. Nature 465, 322

The SN2005E family: 09dav40kpc from putative spiral hostAbs R mag ~-15Fast: 1 mag in 10 dayVery red, g-r = 1.2

Similar to SN1991bg but with HeHydrogen in nebular phase

Kasliwal et al., in prep.Sullivan et al., in prep.

The SN2005E family: 10iuv

37 kpc from putative hostAbs R. mag ~ -15.Fast: 1 mag in 10 daysIntriguing Nebular Spectra

Kasliwal et al., in prep.

Luminous supernovae

Galactic: 51 dwarf novae; 2 AM CVn;…

Luminous supernovaeQuimby et al., 0910.0059

Shock breakout / PTF

PTF detects SNe early -> can detect shock breakout (but still limited by cadence).

GALEX + PTF synergy

PTF + rapid follow up with Swift/UVOT/XRT

Shock breakout / PTFO

fek et al., Apj in press

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Shock breakout / PTFPTF 09dah

NGTFThinking about the next project…

PTF-2 will have a ~30-40 deg2 cameraMounted on the 48” schmidt telescope

Simple scheduling – one day cadence objective: find them young

~8000 deg2 day-1

Scheduled for 2014

EndThank you!

Shock breakout / Intro

Photons first emerge from SN (breakout) when they diffuse ahead of the shockfaster than the shock propogates

Happens at optical depth: =c/v

duration: ~r/c

Decay time: ~r/v

Fast supernovae: 10bhpKasliwal et al., ApJ 723, 98

Very fast: decay ~5 days, MR~-17(e.g., similar to SN200bj, [Poznanski+10])

Fast supernovae: 10bhpKasliwal et al., ApJ 723, 98

If powered by 56Ni then Ni mass ~0.02 Msun and SN quickly becomes optically thin to -rays.

AIC (?).Ia (?)

Luminous red novaPTF 10fqs in M99

Kasliwal et al., 1005.1455

Faint/slow event in M99: MR~-11

PTF 10fqsKasliwal et al., 1005.1455

~10,000 km/s (?)

Search for SB in Chandra archive with Mike Muno

Downloaded the entire Chandra archive

Search for transients and highly variableObjects (on short time scale)

First pass completed: complete for events brighter than 40 counts

No SN 2008D-like events (Soderberg et al. 2008)

Next: calc. efficiency and extend to faint sources

Relative photometrySolution using linear least squares

mij – instrumental mag

i-star (1..p), j-image (1..q)

Solving per field (overlap between fields not guaranteed)

ij – instrumental mag err

ijij zmm

Relative photometryUsing linear least squares

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Observations

Free p

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ijij zmm

Relative photometrySolution using linear least squares

ijij zmm

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ij ij

We need to solve (in the presence of errors):

Relative photometrySimultaneous absolute calibration

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P H is (pq)x(p+q) matrixHowever, rank is p+q-1

jM

M1

100

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000 Adding calibration block

Relative photometryAdditional de-trending

We can add more columns to H and P.For example: Airmass x color term

Positional terms

Multiple CCDs (i.e, overlap)

obsbm

First results from The Palomar Transient Factory Eran Ofek Einstein fellow CALTECH.

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Transcript of First results from The Palomar Transient Factory Eran Ofek Einstein fellow CALTECH.