Index: trunk/doc/release.2015/ps1.diffs/Makefile =================================================================== --- trunk/doc/release.2015/ps1.diffs/Makefile (revision 40694) +++ trunk/doc/release.2015/ps1.diffs/Makefile (revision 40695) @@ -2,5 +2,5 @@ DO_PDFLATEX = 1 -DO_BIBTEX = 1 +DO_BIBTEX = 0 help: @@ -17,12 +17,26 @@ ../inputs/astro.sty \ ../inputs/apj.bst \ +../inputs/code.sty \ diffs.tex \ -references.bib \ -apj-jour.bib \ +diffs.bbl \ figures/noise_model/variance.eps \ figures/noise_model/covariance.eps \ figures/stack/stack_image.eps \ figures/all/kernel.eps \ -figures/all/sn2009kf.eps +figures/all/sn2009kf.eps \ +figures/diff/stamps_mean.eps \ +figures/diff/stamps_rms.eps \ +figures/diff/kernel_x.eps \ +figures/diff/kernel_xx.eps \ +figures/diff/kernel_xy.eps \ +figures/diff/deconv_max.eps \ +figures/noise_model/input_phot.eps \ +figures/noise_model/warp_phot.eps \ +figures/noise_model/diff_phot.eps \ +figures/noise_model/stack_phot.eps \ +figures/stack/stack_conv_m_dm.eps \ +figures/stack/stack_unconv_m_dm.eps \ +figures/stack/stack_conv_hist.eps \ +figures/stack/stack_unconv_hist.eps include ../Makefile.Common @@ -30,2 +44,4 @@ # submission : # tar --transform 's%inputs/%%' -zcf waters2017.tgz $(FILES) + +detrend.tgz: $(FILES) Index: trunk/doc/release.2015/ps1.diffs/diffs.tex =================================================================== --- trunk/doc/release.2015/ps1.diffs/diffs.tex (revision 40694) +++ trunk/doc/release.2015/ps1.diffs/diffs.tex (revision 40695) @@ -63,11 +63,30 @@ \section{Introduction} -The age of synoptic surveys has come. As optical (and other -wavelength) telescopes are surveying ever increasing areas to ever -fainter flux limits with multiple repeats, there is a growing interest -in the study of transient phenomena. This technological progress is -well matched with the current scientific emphases on large samples of -supernovae (SN), microlenses, asteroids, and other transients and -variable sources. +The past three decades have seen the increasing importance of +time-domain surveys in astronomy. These include asteroid searches +such as the Lincoln Near-Earth Asteroid Research +\citep[LINEAR][]{2000Icar..148...21S}, the Lowell Observatory +Near-Earth Object Search \citep[LONEOS,][]{1995DPS....27.0110B}, the +Catalina Sky Survey \citep{2003DPS....35.3604L}, and ATLAS +\citep{2018PASP..130f4505T}; microlensing surveys such as MACHO +\citep{1993ASPC...43..291A} and Optical Gravitational Lens Experiment +\citep[OGLE,][]{1992AcA....42..253U}; and searches for supernovae and +other transient sources such as ASAS-SN \citep{2014ApJ...788...48S}, the +Palomar Transient Factory \citep[PTF,][]{2009PASP..121.1395L}, and the Robotic Optical +Transient Search Experiment \citep[ROTSE-I,][]{2000ApJ...542..251A}. + +The Pan-STARRS Observatory \citep{chambers2017} has been a leader in +the searches for both explosive transient / supernova and potentially +hazardous asteroids. According to the statistics maintained by David +Bishop\footnote{http://www.rochesterastronomy.org/snimages/archives.html}, +since 2009, 40\% of all supernova have been discovered by +Pan-STARRS\,1. Similarly, 24\% of all Near Earth Objects (NEOs) +discovered to date have been found by +Pan-STARRS\footnote{https://cneos.jpl.nasa.gov/stats/site\_all.html}. +Since 2014, when Pan-STARRS shifted its primary mission to the search +for NEOs, this fraction has increased to 41\%. Both of these search +programs use nightly observations to hunt for features which have +changed, either between multiple images in a single night or between +the current image and an archival reference image. PSF-matched image differencing\footnote{We eschew the popular term @@ -88,5 +107,5 @@ of the convolution kernel as a linear combination of basis functions, which allows the least-squares problem to be reduced to a matrix -equation. \citet{2000A&AS..144..363A} showed how this can be expanded +equation. \citet{2000AAS..144..363A} showed how this can be expanded to allow spatial variation of the kernel across the images. Of course, the basis functions used for the kernel may be completely @@ -137,5 +156,5 @@ basis functions, $g_i(x,y) k_i(u,v)$, where the inclusion of $g_i(x,y)$ allows for spatial variation of the kernel. In order to -enforce conservation of flux \citep[following][]{2000A&AS..144..363A}, +enforce conservation of flux \citep[following][]{2000AAS..144..363A}, we specify that all of the kernel basis functions have zero sum, $\sum_{u,v} k_i(u,v) = 0\ \forall i$. This may be achieved by scaling @@ -161,10 +180,10 @@ $\chi^2$ between wide and narrow kernels. Setting $c_i \equiv 0$ and $p_i \equiv 0$ reduces the above equation to the -\citet{2000A&AS..144..363A} formalism, but with the normalisation +\citet{2000AAS..144..363A} formalism, but with the normalisation ($b_0$) included explicitly. In practise, the above sum will only be over small regions (known as ``stamps''), and if we assume that the spatial variation is not large, then we can simply use the coordinates of the stamp centres for the $g_i(x,y)$; this allows a faster -calculation \citep{2000A&AS..144..363A}. +calculation \citep{2000AAS..144..363A}. To simplify the equation, we write @@ -199,5 +218,5 @@ other special polynomial for the $f_i(x,y)$ and $g_i(x,y)$ is simple and convenient. The kernel basis function sets of -\citet{1998ApJ...503..325A} and \citet{2000A&AS..144..363A} are +\citet{1998ApJ...503..325A} and \citet{2000AAS..144..363A} are \begin{equation} g_i(x,y) k_i'(u,v) = \psi_i x^\ell y^m u^p v^q \exp((u^2+v^2)/2s_i^2) @@ -338,11 +357,13 @@ \subsection{Stamps} -The choice of stamps is key to successful PSF-matching --- the -convolution kernel is only as good as the stamps used to construct it. -We use a merged list of sources from photometry of the two input -images as the basis of our stamps list. Sources with a flag -indicating that it is anything other than a pristine astrophysical -source are excluded. At the present time, we make no effort to select -sources of a particular color or range of colors. +Since we restrict the analysis of the kernel required for PSF matching +to the small ``stamps'' centered on bright stars, the choice of stamps +is key to successful PSF-matching. The convolution kernel is only as +good as the stamps used to construct it. We use a merged list of +sources from photometry of the two input images as the basis of our +stamps list. Sources with a flag indicating that it is anything other +than a pristine astrophysical source are excluded. At the present +time, we make no effort to select sources of a particular color or +range of colors. We exclude sources with any masked pixels that would affect the @@ -490,5 +511,5 @@ progressive software packages producing \citep[e.g., SWarp:][]{2002ASPC..281..228B} and using \citep[e.g., - SExtractor:][]{1996A&AS..117..393B} weight maps to characterise the + SExtractor:][]{1996AAS..117..393B} weight maps to characterise the noise over the image. Because of simplicity and lower calculation cost relative to weights or standard deviations, we prefer to @@ -993,5 +1014,6 @@ \clearpage \bibliographystyle{apj} -\bibliography{apj-jour,references} +%\bibliography{apj-jour,references} +\input{diffs.bbl} \end{document} Index: trunk/doc/release.2015/ps1.diffs/references.bib =================================================================== --- trunk/doc/release.2015/ps1.diffs/references.bib (revision 40694) +++ trunk/doc/release.2015/ps1.diffs/references.bib (revision 40695) @@ -1,4 +1,186 @@ -@ARTICLE{2000A&AS..144..363A, +@ARTICLE{2000ApJ...542..251A, + author = {{Akerlof}, C. and {Balsano}, R. and {Barthelmy}, S. and {Bloch}, J. and + {Butterworth}, P. and {Casperson}, D. and {Cline}, T. and {Fletcher}, S. and + {Gisler}, G. and {Hills}, J. and {Kehoe}, R. and {Lee}, B. and + {Marshall}, S. and {McKay}, T. and {Pawl}, A. and {Priedhorsky}, W. and + {Seldomridge}, N. and {Szymanski}, J. and {Wren}, J.}, + title = "{Rapid Optical Follow-up Observations of SGR Events with ROTSE-I}", + journal = {\apj}, + keywords = {Gamma Rays: Bursts, Gamma Rays: Observations, pulsars: individual (SGR 1900+14, SGR 1806-20)}, + year = 2000, + month = oct, + volume = 542, + pages = {251-256}, + doi = {10.1086/309535}, + adsurl = {http://adsabs.harvard.edu/abs/2000ApJ...542..251A}, + adsnote = {Provided by the SAO/NASA Astrophysics Data System} +} + +@ARTICLE{2009PASP..121.1395L, + author = {{Law}, N.~M. and {Kulkarni}, S.~R. and {Dekany}, R.~G. and {Ofek}, E.~O. and + {Quimby}, R.~M. and {Nugent}, P.~E. and {Surace}, J. and {Grillmair}, C.~C. and + {Bloom}, J.~S. and {Kasliwal}, M.~M. and {Bildsten}, L. and + {Brown}, T. and {Cenko}, S.~B. and {Ciardi}, D. and {Croner}, E. and + {Djorgovski}, S.~G. and {van Eyken}, J. and {Filippenko}, A.~V. and + {Fox}, D.~B. and {Gal-Yam}, A. and {Hale}, D. and {Hamam}, N. and + {Helou}, G. and {Henning}, J. and {Howell}, D.~A. and {Jacobsen}, J. and + {Laher}, R. and {Mattingly}, S. and 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{Szczygie{\l}}, D.~M. and {Brimacombe}, J. and {Adams}, S. and + {Campillay}, A. and {Choi}, C. and {Contreras}, C. and {Dietrich}, M. and + {Dubberley}, M. and {Elphick}, M. and {Foale}, S. and {Giustini}, M. and + {Gonzalez}, C. and {Hawkins}, E. and {Howell}, D.~A. and {Hsiao}, E.~Y. and + {Koss}, M. and {Leighly}, K.~M. and {Morrell}, N. and {Mudd}, D. and + {Mullins}, D. and {Nugent}, J.~M. and {Parrent}, J. and {Phillips}, M.~M. and + {Pojmanski}, G. and {Rosing}, W. and {Ross}, R. and {Sand}, D. and + {Terndrup}, D.~M. and {Valenti}, S. and {Walker}, Z. and {Yoon}, Y. + }, + title = "{The Man behind the Curtain: X-Rays Drive the UV through NIR Variability in the 2013 Active Galactic Nucleus Outburst in NGC 2617}", + journal = {\apj}, +archivePrefix = "arXiv", + eprint = {1310.2241}, + primaryClass = "astro-ph.HE", + keywords = {galaxies: active, galaxies: nuclei, galaxies: Seyfert, line: formation, line: profiles}, + year = 2014, + month = jun, + volume = 788, + eid = {48}, + pages = {48}, + doi = {10.1088/0004-637X/788/1/48}, + adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...788...48S}, + adsnote = {Provided by the SAO/NASA Astrophysics Data System} +} + +@ARTICLE{1992AcA....42..253U, + author = {{Udalski}, A. and {Szymanski}, M. and {Kaluzny}, J. and {Kubiak}, M. and + {Mateo}, M.}, + title = "{The Optical Gravitational Lensing Experiment}", + journal = {\actaa}, + keywords = {Charge Coupled Devices, Galactic Bulge, Gravitational Lenses, Star Distribution, Statistical Analysis, Galactic Clusters, Galactic Halos, Variable Stars}, + year = 1992, + volume = 42, + pages = {253-284}, + adsurl = {http://adsabs.harvard.edu/abs/1992AcA....42..253U}, + adsnote = {Provided by the SAO/NASA Astrophysics Data System} +} + +@INPROCEEDINGS{1993ASPC...43..291A, + author = {{Alcock}, C. and {Allsman}, R.~A. and {Axelrod}, T.~S. and {Bennett}, D.~P. and + {Cook}, K.~H. and {Park}, H.~S. and {Marshall}, S.~L. and {Stubbs}, C.~W. and + {Griest}, K. and {Perlmutter}, S. and 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