Astronomy 255 / Physics 295
Research Methods in Astrophysics
Professor Marla Geha
http://astro.yale.edu/mgeha/A255
Prof. K’s Research
What do Astronomers/Astrophysicists do?
Loose Categories of Astronomers
•
Observers / Data Miners
-- Go to telescopes, take data to observe new objects/phenomena
-- Mine existing large databases to find new objects/phenomena
-- Test the predictions/ideas of the modelers/simulators/theorists
•
Modelers/Simulators/Theorists
Observers
Most professional research is conducted on telescopes which are either privately or nationally
owned. Researchers write proposals to request a certain number of nights/hours.
Las Campanas, Chile
Mauna Kea, Hawaii
Kitt Peak, AZ
Professional astronomy is done exclusively
on computers-- from taking data to
processing results and writing papers.
2013
1850
Magellan telescope control room, Chile
Maria Mitchell, Nantucket
LBT
Twin 8.4m telescopes
Mt. Graham, Arizona
UVa is a partner
and gets
guaranteed time
in nights per
year
Also get time on 6.5m class telescopes (Chile and
Arizona), Steward and APO facilities, ALMA
Our class has been
granted half a night
at APO, New
Mexico.
In lieu of a final, you will write an observing proposal
to compete for this time. Proposals will be evaluated
“TAC style” by you all on the last day of class.
(Remote) observations for best project will be taken
(weather permitting) on the night of May 8.
Two types of efforts in the community: survey style data
collection (SDSS, LSST), and PI-driven projects.
The Sloan Digital Sky Survey (SDSS)
2.5-meter SDSS telescope, New Mexico
The first (and so far only so) systematic,
digital mapping of the sky was completed a
few years ago: SDSS.
Data is accessed entirely via online webtools.
Much of the remainder of this class
will be devoted to Database
techniques
The Sloan Digital Sky Survey (SDSS)
Camera used to take astronomical
images are similar to cell phones...
iPhone 4: 5 Megapixel
... just slightly bigger
SDSS Camera: 120 Megapixels
(built in 1998!!)
SLOAN DIGITAL SKY SURVEY III
SkyServer
Home
Data
DR9 Tools
Schema
DR9
Education
Astronomy
SDSS
HTML
Data accessed via web
tools and available to
everyone.
Imaging
Visual Tools
- Imaging Query
CSV
(Shift-mouse to select multiple contiguous entries, Ctrl-mouse to select non-contiguous entries)
Scrolling sky
- SQL
Reset Form
XML
Parameters to return
Get images
- Rectangular
Help
Please see the Query Limits help page for timeouts and row limits. To get FITS files
from the Science Archive Server (SAS), please use the button(s) on the query results page.
Famous places
- Radial
Site Search
Limit number of output rows (0 for max) to 50
Output Format
Search
Download
Imaging Query Form
Submit Request
Getting Started
Contact Us
Spectroscopy
minimal
typical
radec
model_mags
model_magerrs
none
minimal
typical
radec
Submit Request
Reset Form
- Spectro Query
Position Constraints
Object Crossid
CasJobs
min
ra
dec
max
ra
dec
center
ra
Rectangle
(max 10 square degrees)
Cone
dec 0.2
180.0
List of ra, dec[, radius]
radius 5.0 arcmin (max 30')
Nearest Only
(max 100 obj)
ra,dec,sep
256.443154,58.0255,1.0
29.94136,0.08930,1.0
Proximity
We will work with
these data in Lab 6.
radius 1.0 arcmin (max 10')
Upload File
Choose File
None
All Nearby
No position constraint
no file selected
Submit Request
Reset Form
Imaging Constraints
Magnitude and Color Type
Petro
Model
PSF
min
u
g
r
i
z
max
u
g
r
i
z
min
u-g
g-r
r-i
i-z
max
u-g
g-r
r-i
i-z
Magnitudes
Colors
Obj Type
Extended Sources (e.g., Galaxies)
Sky
Hubble Space Telescope (HST)
2.4-meter primary mirror in orbit
We will work with HST data in HW #2.
MAST
STScI
HST Home
Tools
About HST
Mission_Search
Getting Started
Tutorial
Registration
Search Website
Archive Status
Follow Us
HST Search
HSTonline Search
HST Search Form
Archive Status
Help
Field Descriptions
Standard Form
File Upload Form
Search
Reset
Target Name
Clear Form
Resolver
Radius (arcmin)
Resolve
Right Ascension
3.0
Declination
Equinox
J2000
Imagers
ALL
Spectrographs
NONE
ALL
NONE
Other
ALL
NONE
STIS
STIS
FGS
NICMOS
NICMOS
HSP
WFPC2
GHRS
WF/PC
FOS
FOC
FOC
ACS
ACS
WFC3
WFC3
COS
COS
User-specified field 1
Start Time
Exp Time
Proposal ID
Release Date
Dataset
Filters/Gratings
Obset ID
Archive Date
Target Descrip
Apertures
Observations
Science
Calibration
PI Last Name
Field Descriptions
User-specified field 2
Dataset
Field Descriptions
Dataset
Sort By:
Output Columns
Mark
Dataset
Target Name
RA (J2000)
Dec (J2000)
Ref
Start Time
Stop Time
Exp Time
Instrument
Apertures
add
Mark
up
ang_sep (')
Reverse
Target Name
Reverse
Dataset
Reverse
down
Output Coords :
Sexagesimal
Hours
Output Format
HTML_Table
reset
Make Rows Distinct
add all
Maximum Records:
Records per Page:
Search
Degrees
remove
Reset
Skip formatting
5001
500
Clear Form
Loose Categories of Astronomers
•
Observers / Data Miners
-- Go to telescopes, take data to observe new objects/phenomena
-- Mine existing large databases to find new objects/phenomena
-- Test the predictions/ideas of the modelers/simulators/theorists
•
Modelers/Simulators/Theorists
-- Explain the observations of the Observers
-- Run computer simulations to explain new objects/phenomena
-- Use physics to explain new objects/phenomena
Simulating the Universe
Loose Categories of Astronomers
•
Observers / Data Miners
-- Go to telescopes, take data to observe new objects/phenomena
-- Mine existing large databases to find new objects/phenomena
-- Test the predictions/ideas of the modelers/simulators/theorists
•
Modelers/Simulators/Theorists
-- Explain the observations of the Observers
-- Run computer simulations to explain new objects/phenomena
-- Use physics to explain new objects/phenomena
These are just examples.
The exciting stuff is always on the boundaries.
•
This “half” of the class will also serve as your
introduction to “Astronomer 101”:
•
ADS: http://adsabs.harvard.edu/
abstract_service.html
•
•
Astro-ph: http://xxx.lanl.gov/archive/astro-ph
•
•
Astrobetter: http://www.astrobetter.com
@Awesome_Ph (summarizes interesting astro-ph
articles each day in 140 characters or less.)
We will begin each class with an abstract.
• A major effort in present day Astronomy
(both observers and theorists) is in the
area of surveys <==> databases.
• Automated imaging/spectroscopy of large
swaths of sky with dedicated telescopes
and instruments.
• Specific observing strategy chosen to
optimize a set of science questions.
Home
SDSS-III
SDSS Data DR10
SDSS Data DR9
SDSS Data DR8
SDSS Data DR7
Science
Press Releases
Education
Image Gallery
Legacy Survey
SEGUE
Supernova Survey
Collaboration
Publications
Contact Us
Search
Images of the
SDSS
The Sloan Digital Sky Survey
(click for more information)
The Sloan Digital Sky Survey (SDSS) is one of the
most ambitious and influential surveys in the history of
astronomy. Over eight years of operations (SDSS-I,
2000-2005; SDSS-II, 2005-2008), it obtained deep,
multi-color images covering more than a quarter of the
sky and created 3-dimensional maps containing more
than 930,000 galaxies and more than 120,000 quasars.
SDSS data have been released to the scientific
community and the general public in annual
increments, with the final public data release from
SDSS-II occurring in October 2008. That release, Data
Release 7, is available through this website.
The Final Survey
Meanwhile, SDSS is continuing with the Third Sloan
Digital Sky Survey (SDSS-III), a program of four new
surveys using SDSS facilities. SDSS-III began
observations in July 2008 and released Data Release 8
in January 2011, Data Release 9 in August 2012, and
Data Release 10 in July 2013. SDSS-III will continue
operating and releasing data through 2014.
Data Release 10 contains the first release of APOGEE
infrared Galactic spectroscopy as well as cumulative
updates to the BOSS optical extragalactic spectroscopy
archive.
Data Release 9 contains the first release of BOSS
spectroscopy to the public as well as several significant
updates to the cumulative SDSS archive.
Data Release 8 contains all images from the SDSS
telescope - the largest color image of the sky ever
made. It also includes measurements for nearly 500
million stars and galaxies, and spectra of nearly two
million. All the images, measurements, and spectra are
The Whirlpool Galaxy (M51)
The SDSS used a dedicated 2.5-meter telescope at
Apache Point Observatory, New Mexico, equipped
with two powerful special-purpose instruments. The
120-megapixel camera imaged 1.5 square degrees of
sky at a time, about eight times the area of the full
moon. A pair of spectrographs fed by optical fibers
measured spectra of (and hence distances to) more than
600 galaxies and quasars in a single observation. A
custom-designed set of software pipelines kept pace
with the enormous data flow from the telescope. The
two key technologies that enabled the SDSS, optical
fibers and the digital imaging detectors known as
CCDs, were the discoveries awarded the 2009 Nobel
Prize in Physics.
The SDSS Field of Streams
During its first phase of operations, 2000-2005, the
SDSS imaged more than 8,000 square degrees of the
sky in five optical bandpasses, and it obtained spectra
of galaxies and quasars selected from 5,700 square
degrees of that imaging. It also obtained repeated
imaging (roughly 30 scans) of a 300 square degree
stripe in the southern Galactic cap.
With new financial support and an expanded
collaboration including 25 institutions around the
globe, SDSS-II carried out three distinct surveys:
The Sloan Legacy Survey completed the original
SDSS imaging and spectroscopic goals. The final
dataset includes 230 million celestial objects
detected in 8,400 square degrees of imaging and
spectra of 930,000 galaxies, 120,000 quasars,
and 225,000 stars.
SEGUE (the Sloan Extension for Galactic
Understanding and Exploration) probed the
structure and history of the Milky Way galaxy,
with new imaging of 3500 square degrees and
spectra of 240,000 stars in a variety of categories
in selected fields.
The Sloan Supernova Survey carried out repeat
imaging of the 300 square degree southern
equatorial stripe to discover and measure
supernovae and other variable objects. In the
course of three 3-month campaigns, the
supernova survey discovered nearly 500
spectroscopically confirmed Type Ia supernovae,
which are being used to determine the history of
the accelerating cosmic expansion over the last 4
billion years.
SDSS data have supported fundamental work across an
extraordinary range of astronomical disciplines,
including the properties of galaxies, the evolution of
quasars, the structure and stellar populations of the
Milky Way, the dwarf galaxy companions of the Milky
Way and M31, asteroids and other small bodies in the
SDSS-II Supernovae
Quasar Spectra
Contact Us
Search
SDSS data have been released to the scientific
community and the general public in annual
increments, with the final public data release from
SDSS-II occurring in October 2008. That release, Data
Release 7, is available through this website.
The Final Survey
Meanwhile, SDSS is continuing with the Third Sloan
Digital Sky Survey (SDSS-III), a program of four new
surveys using SDSS facilities. SDSS-III began
observations in July 2008 and released Data Release 8
in January 2011, Data Release 9 in August 2012, and
Data Release 10 in July 2013. SDSS-III will continue
operating and releasing data through 2014.
Data Release 10 contains the first release of APOGEE
infrared Galactic spectroscopy as well as cumulative
updates to the BOSS optical extragalactic spectroscopy
archive.
The Whirlpool Galaxy (M51)
Data Release 9 contains the first release of BOSS
spectroscopy to the public as well as several significant
updates to the cumulative SDSS archive.
Data Release 8 contains all images from the SDSS
telescope - the largest color image of the sky ever
made. It also includes measurements for nearly 500
million stars and galaxies, and spectra of nearly two
million. All the images, measurements, and spectra are
available free online. You can browse through sky
images, look up data for individual objects, or search
for objects anywhere in the sky based on any criteria.
The SDSS
SDSS used
used aa dedicated
dedicated2.5-meter
2.5-metertelescope
telescopeatat
The
Apache Point Observatory, New Mexico, equipped
with two powerful special-purpose instruments. The
120-megapixel camera imaged 1.5 square degrees of
sky at a time, about eight times the area of the full
moon. A pair of spectrographs fed by optical fibers
measured spectra of (and hence distances to) more than
600 galaxies and quasars in a single observation. A
custom-designed set of software pipelines kept pace
with the enormous data flow from the telescope. The
two key technologies that enabled the SDSS, optical
fibers and the digital imaging detectors known as
CCDs, were the discoveries awarded the 2009 Nobel
Prize in Physics.
SDSS Galaxy Map
The SDSS Field of Streams
During its first phase of operations, 2000-2005, the
SDSS imaged more than 8,000 square degrees of the
sky in five optical bandpasses, and it obtained spectra
of galaxies and quasars selected from 5,700 square
degrees of that imaging. It also obtained repeated
imaging (roughly 30 scans) of a 300 square degree
stripe in the southern Galactic cap.
With new financial support and an expanded
collaboration including 25 institutions around the
globe, SDSS-II carried out three distinct surveys:
SDSS-II Supernovae
An Intro to the Sloan Digital Sky Survey
An Intro to the Sloan Digital Sky Survey
•
Imaged the sky in 5 filters in
“drift scan” mode: tracks great
circles at the sidereal rate
(54.1s per filter; 18.75 deg^2
imaged per hour).
•
Automated pipeline: determine
astrometric calibration and
detect and measure the
brightnesses, positions, and
shapes of objects.
•
Objects are then chosen for
spectroscopy: 640-fiber-fed pair
of multiobject double
spectrographs, giving coverage
from 3800 Å to 9200 Å at a
resolution of λ/Δλ ≃ 2000.
Draft version January 20, 2014
Preprint typeset using LATEX style emulateapj v. 12/16/11
arXiv:1307.7735v3 [astro-ph.IM] 17 Jan 2014
THE TENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST SPECTROSCOPIC DATA
FROM THE SDSS-III APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT
Christopher P. Ahn1 , Rachael Alexandroff2 , Carlos Allende Prieto3,4 , Friedrich Anders5,6 ,
Scott F. Anderson7 , Timothy Anderton1 , Brett H. Andrews8 , Éric Aubourg9 , Stephen Bailey10 ,
Fabienne A. Bastien11 , Julian E. Bautista9 , Timothy C. Beers12,13 , Alessandra Beifiori14 , Chad F. Bender15,16
Andreas A. Berlind11 , Florian Beutler10 , Vaishali Bhardwaj7,10 , Jonathan C. Bird11 , Dmitry Bizyaev17,18 ,
Cullen H. Blake19 , Michael R. Blanton20 , Michael Blomqvist21 , John J. Bochanski22,7 , Adam S. Bolton1 ,
Arnaud Borde23 , Jo Bovy24,25 , Alaina Shelden Bradley17 , W. N. Brandt15,26 , Dorothée Brauer5 , J. Brinkmann17 ,
Joel R. Brownstein1 , Nicolás G. Busca9 , William Carithers10 , Joleen K. Carlberg27 , Aurelio R. Carnero28,29 ,
Michael A. Carr30 , Cristina Chiappini5,29 , S. Drew Chojnowski31 , Chia-Hsun Chuang32 , Johan Comparat33 ,
Justin R. Crepp34 , Stefano Cristiani35,36 , Rupert A.C. Croft37 , Antonio J. Cuesta38 , Katia Cunha28,39 ,
Luiz N. da Costa28,29 , Kyle S. Dawson1 , Nathan De Lee11 , Janice D. R. Dean31 , Timothée Delubac23 ,
Rohit Deshpande15,16 , Saurav Dhital40,11 , Anne Ealet41 , Garrett L. Ebelke17,18 , Edward M. Edmondson42 ,
Daniel J. Eisenstein43 , Courtney R. Epstein8 , Stephanie Escoffier41 , Massimiliano Esposito3,4 ,
Michael L. Evans7 , D. Fabbian3 , Xiaohui Fan39 , Ginevra Favole32 , Bruno Femenı́a Castellá3,4 ,
Emma Fernández Alvar3,4 , Diane Feuillet18 , Nurten Filiz Ak15,26,44 , Hayley Finley45 , Scott W. Fleming15,16 ,
Andreu Font-Ribera46,10 , Peter M. Frinchaboy47 , J. G. Galbraith-Frew1 , D. A. Garcı́a-Hernández3,4 ,
Ana E. Garcı́a Pérez31 , Jian Ge48 , R. Génova-Santos3,4 , Bruce A. Gillespie2,17 , Léo Girardi49,29 ,
Jonay I. González Hernández3 , J. Richard Gott, III30 , James E. Gunn30 , Hong Guo1 , Samuel Halverson15 ,
Paul Harding50 , David W. Harris1 , Sten Hasselquist18 , Suzanne L. Hawley7 , Michael Hayden18 ,
Frederick R. Hearty31 , Artemio Herrero Davó3,4 , Shirley Ho37 , David W. Hogg20 , Jon A. Holtzman18 ,
Klaus Honscheid51,52 , Joseph Huehnerhoff17 , Inese I. Ivans1 , Kelly M. Jackson47,53 , Peng Jiang54,48 ,
Jennifer A. Johnson8,52 , K. Kinemuchi17,18 , David Kirkby21 , Mark A. Klaene17 , Jean-Paul Kneib55,33 ,
Lars Koesterke56 , Ting-Wen Lan2 , Dustin Lang37 , Jean-Marc Le Goff23 , Alexie Leauthaud57 , Khee-Gan Lee58 ,
Young Sun Lee18 , Daniel C. Long17,18 , Craig P. Loomis30 , Sara Lucatello49 , Robert H. Lupton30 , Bo Ma48 ,
Claude E. Mack III11 , Suvrath Mahadevan15,16 , Marcio A. G. Maia28,29 , Steven R. Majewski31 ,
Elena Malanushenko17,18 , Viktor Malanushenko17,18 , A. Manchado3,4 , Marc Manera42 , Claudia Maraston42 ,
Daniel Margala21 , Sarah L. Martell59 , Karen L. Masters42 , Cameron K. McBride43 , Ian D. McGreer39 ,
Richard G. McMahon60,61 , Brice Ménard2,57,62 , Sz. Mészáros3,4 , Jordi Miralda-Escudé63,64 , Hironao Miyatake30 ,
Antonio D. Montero-Dorta1 , Francesco Montesano14 , Surhud More57 , Heather L. Morrison50 , Demitri Muna8 ,
Jeffrey A. Munn65 , Adam D. Myers66 , Duy Cuong Nguyen67 , Robert C. Nichol42 , David L. Nidever68,31 ,
Pasquier Noterdaeme45 , Sebastián E. Nuza5 , Julia E. O’Connell47 , Robert W. O’Connell31 , Ross O’Connell37 ,
Matthew D. Olmstead1 , Daniel J. Oravetz17 , Russell Owen7 , Nikhil Padmanabhan38 ,
Nathalie Palanque-Delabrouille23 , Kaike Pan17 , John K. Parejko38 , Prachi Parihar30 , Isabelle Pâris69 ,
Joshua Pepper70,11 , Will J. Percival42 , Ignasi Pérez-Ràfols64,71 , Hélio Dotto Perottoni72,29 ,
Patrick Petitjean45 , Matthew M. Pieri42 , M. H. Pinsonneault8 , Francisco Prada73,32,74 ,
Adrian M. Price-Whelan75 , M. Jordan Raddick2 , Mubdi Rahman2 , Rafael Rebolo3,76 , Beth A. Reid10,25 ,
Jonathan C. Richards1 , Rogério Riffel77,29 , Annie C. Robin78 , H. J. Rocha-Pinto72,29 , Constance M. Rockosi79 ,
Natalie A. Roe10 , Ashley J. Ross42 , Nicholas P. Ross10 , Graziano Rossi23 , Arpita Roy15 , J. A. Rubiño-Martin3,4 ,
Cristiano G. Sabiu80 , Ariel G. Sánchez14 , Bası́lio Santiago77,29 , Conor Sayres7 , Ricardo P. Schiavon81 ,
David J. Schlegel10 , Katharine J. Schlesinger82 , Sarah J. Schmidt8 , Donald P. Schneider15,26 ,
Mathias Schultheis78 , Kris Sellgren8 , Hee-Jong Seo10 , Yue Shen43,83 , Matthew Shetrone84 , Yiping Shu1 ,
Audrey E. Simmons17 , M. F. Skrutskie31 , Anže Slosar85 , Verne V. Smith12 , Stephanie A. Snedden17 ,
Jennifer S. Sobeck86 , Flavia Sobreira28,29 , Keivan G. Stassun11,87 , Matthias Steinmetz5 , Michael A. Strauss30,88 ,
Alina Streblyanska3,4 , Nao Suzuki10 , Molly E. C. Swanson43 , Ryan C. Terrien15,16 , Aniruddha R. Thakar2 ,
Daniel Thomas42 , Benjamin A. Thompson47 , Jeremy L. Tinker20 , Rita Tojeiro42 , Nicholas W. Troup31 ,
Jan Vandenberg2 , Mariana Vargas Magaña37 , Matteo Viel35,36 , Nicole P. Vogt18 , David A. Wake89 ,
Benjamin A. Weaver20 , David H. Weinberg8 , Benjamin J. Weiner39 , Martin White90,10 , Simon D.M. White91 ,
John C. Wilson31 , John P. Wisniewski92 , W. M. Wood-Vasey93,88 , Christophe Yèche23 , Donald G. York94 ,
O. Zamora3,4 , Gail Zasowski8,2 , Idit Zehavi50 , Gong-Bo Zhao42,95 , Zheng Zheng1 , Guangtun Zhu2
As an introduction to science writing,
we will start each class discussing an
abstract from a professional journal
or observing proposal.
Draft version January 20, 2014
ABSTRACT
The Sloan Digital Sky Survey (SDSS) has been in operation since 2000 April. This paper presents the
tenth public data release (DR10) from its current incarnation, SDSS-III. This data release includes the
first spectroscopic data from the Apache Point Observatory Galaxy Evolution Experiment (APOGEE),
along with spectroscopic data from the Baryon Oscillation Spectroscopic Survey (BOSS) taken through
2012 July. The APOGEE instrument is a near-infrared R ⇠ 22,500 300-fiber spectrograph covering
1.514–1.696 µm. The APOGEE survey is studying the chemical abundances and radial velocities of
roughly 100,000 red giant star candidates in the bulge, bar, disk, and halo of the Milky Way. DR10
includes 178,397 spectra of 57,454 stars, each typically observed three or more times, from APOGEE.
Derived quantities from these spectra (radial velocities, e↵ective temperatures, surface gravities, and
metallicities) are also included.
The Astrophysical Journal Supplement Series, 182:543–558, 2009 June
⃝
C 2009.
doi:10.1088/0067-0049/182/2/543
The American Astronomical Society. All rights reserved. Printed in the U.S.A.
THE SEVENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY
Kevork N. Abazajian1 , Jennifer K. Adelman-McCarthy2 , Marcel A. Agüeros3,102 , Sahar S. Allam2,4 ,
Carlos Allende Prieto5 , Deokkeun An6,7 , Kurt S. J. Anderson8,9 , Scott F. Anderson10 , James Annis2 , Neta
A. Bahcall11 , C. A. L. Bailer-Jones12 , J. C. Barentine13 , Bruce A. Bassett14,15 , Andrew C. Becker10 , Timothy
No. 2, 16
2009
SEVENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY
545
C. Beers , Eric F. Bell12 , Vasily Belokurov17 , Andreas A. Berlind18 , Eileen F. Berman2 , Mariangela Bernardi19 ,
11
8
20
21
10,22
, Dmitry
, JohnTata
P. Blakeslee
, Michael
R.Post
Blanton
, John J.
Bochanski
, William
Steven J. Bickerton
97 National
Centre forBizyaev
Radio Astrophysics,
Institute of Fundamental
Research,
Bag 3, Ganeshkhind,
Pune
411007, India
2
8 and Research Center, Institute
23,24for Astronomy, 34 Ohia
8 Ku St., Pukalani, HI 96768, 25
98 Advanced Technology
, J. Brinkmann , Robert J. Brunner USA
, Tamás Budavári26 ,
N. Boroski , Howard J. Brewington , Jarle Brinchmann
99 Max-Planck-Institut für Astrophysik, Postfach 1, D-85748 Garching, Germany
26
27
Larry N. Carey10 , Samuel Carliles
, Michael
A.Elmhurst
Carr11
, Francisco
J. Castander
, 60126,
DavidUSA
Cinabro28 , A. J. Connolly10 ,
100 Department
of
Physics,
College,
190
Prospect
Ave.,
Elmhurst,
IL
30
2
31
Cunha
, Paul
C. Czarapata
, James
A. Ellis
Davenport
, Ernst
de USA
Haas32 , Ben Dilday33,34,35 ,
István Csabai29 , Carlos E. 101
Enrico Fermi
Institute,
University of Chicago,
5640R.
South
Avenue, Chicago,
IL 60637,
36,37
38
10 March 19; published
17 2009 May 18
38
Received
2008
December
2;
accepted
2009
Mamoru Doi
, Daniel J. Eisenstein , Michael L. Evans , N. W. Evans , Xiaohui Fan , Scott D. Friedman39 ,
2,34,40
, Masataka Fukugita41 , Boris T. Gänsicke42 , Evalyn Gates34 , Bruce Gillespie26 , G. Gilmore17 ,
Joshua A. Frieman
ABSTRACT
2
43
, James E. Gunn11 , Zsuzsanna Györy29 , Patrick B. Hall44 ,
Belinda Gonzalez , Carlos F. Gonzalez2 , Eva K. Grebel
45
46
47 Digital Sky Survey (SDSS),
48
This paper
describesH.the
Seventh, Data
Release
of the Sloan
marking
theHayes
completion
Paul Harding
, Frederick
Harris
Michael
Harvanek
, Suzanne L. Hawley10 , Jeffrey
J. E.
, Timothy
2
of
the
original
goals
of
the
SDSS
and
the
end
of
the
phase
known
as
SDSS-II.
It
includes
11,663
deg
of
imaging
M. Heckman26 , John S. Hendry2 , Gregory2 S. Hennessy49 , Robert B. Hindsley50 , J. Hoblitt51 , Craig J. Hogan2 , David
data, with most of the ∼2000 deg increment over the previous data release lying in regions of low Galactic
W. Hogg21 , Jon A. Holtzman9 , Joseph B. Hyde19 , Shin-ichi Ichikawa52 , Takashi Ichikawa53 , Myungshin Im54 ,
latitude.
for 357 million distinct
objects. The survey also
includes
10 The catalog contains
12 five-band photometry
38
6
55
Sebastianon
Jester
Linhua
Jiangstripe
, Jennifer
Johnson
, Anders
Jorgensen
Mario
Jurić56 ,
Željko Ivezić
repeat ,photometry
a 120◦ ,long,
2.◦ 5 wide
along theA.
celestial
equator
in the M.
Southern
Galactic, Cap,
with
2
34
57
11
41,58
2,40
, R. Kessler
, S. J.asKleinman
R. Knapp
, Kohki
Konishi
, Richard
G. Kron
Stephen
Kent covered
someM.regions
by as many
90 individual, G.
imaging
runs. We
include
a co-addition
of the best
of these ,
8,59
2
60
2
, roughly
Nikolay
Kuropatkin
, Hubert
, 250
Svetlana
Lebedeva
, Myung
Gyoon
Lee54 , Young
Jurek Krzesinski
data, going
2 mag
fainter than
the mainLampeitl
survey over
deg2 . The
survey has
completed
spectroscopy
16 over 9380 deg2 ; the
10 spectroscopy is now61complete over
26 a large contiguous
19,33,34
2
of the Lin
Northern
Galactic
Cap, 8 , Craig
, Daniel
C. Long
Sun Lee , R. French Leger , Sébastien Lépine , Nolan Li , Marcos Lima area, Huan
11
51 are over 1.6 million spectra
8
the gap62that
was present
in previous
data releases.
There
in total,Malanushenko
including
Jon Loveday
, Robert
H. Lupton
, Eugene
Magnier
, Olena Malanushenko8 , Viktor
,
P. Loomis11 , closing
930,000
galaxies,
56,103 120,000 quasars, and
63 460,000 stars. The data
2 release includes improved stellar
64 photometry at low
65
, Bruce Margon , John P. Marriner , David Martı́nez-Delgado , Takahiko Matsubara ,
Rachel Mandelbaum
Galactic latitude.
The astrometry has all
the second version of the
7
30 been recalibrated with
66
45 USNO CCD Astrograph
11
Peregrine M.
McGehee
, Timothy
A. McKay
, Avery
Meiksin
, Heather
L. Morrison
, Fergal
Mullally
, Jeffrey
Catalog,
reducing
the
rms
statistical
errors
at
the
bright
end
to
45
milliarcseconds
per
coordinate.
We further
quantify
46
66,67
2
68
2
69
,
Tara
Murphy
,
Thomas
Nash
,
Ada
Nebot
,
Eric
H.
Neilsen,
Jr.
,
Heidi
Jo
Newberg
,
Peter
A. Munn
a systematic error in bright galaxy photometry due to poor sky determination; this problem is less severe than
60
2,71
26
, Robert
C.majority
Nicholof
,galaxies.
Tom Nicinski
, Atsuko
Nitta57 ,
R.previously
Newman8,70
reported
for the
Finally, we, Maria
describeNieto-Santisteban
a series of improvements
to the spectroscopic
72
8 and improved wavelength
reductions,
better
flat fielding
calibrationOwen
at the10blue
end, Padmanabhan
better processing73,103 ,
, Daniel
J. Oravetz
, Jeremiah P. Ostriker11 , Russell
, Nikhil
Sadanori
Okamuraincluding
8objects with extremely
74 strong narrow emission
11
2improved determination
60 of stellar metallicities.
of
lines,
and
an
Kaike Pan , Changbom Park , George Pauls , John Peoples Jr. , Will J. Percival , Jeffrey R. Pier46 , Adrian
11,76
, Dimitri
, Paul
A. Price51 , Norbert Purger29 , Thomas Quinn10 , M. Jordan Raddick26 , Paola
C. Pope51,75Key
words:Pourbaix
atlases – catalogs
– surveys
12,77
78
79
26
12
, Gordon
T. Richards
Re Fiorentin
Online-only
material:
color figures, Michael W. Richmond , Adam G. Riess , Hans-Walter Rix , Constance
80
19,81
73
82
68
, David J. Schlegel , Donald P. Schneider , Ralf-Dieter Scholz , Matthias
M. Rockosi , Masao Sako
83
R. Schreiber , Axel D. Schwope68 , Uroš Seljak73,84,85 , Branimir Sesar10 , Erin Sheldon21,86 , Kazu Shimasaku72 ,
Valena C. Sibley2 , A. E. Simmons8 , Thirupathi Sivarani16,87 , J. Allyn Smith88 , Martin C. Smith17 , Vernesa Smolčić89 ,
respectively
(Abazajian
et al.
8
2 SURVEY
68
2 2004), although these11values
1. OVERVIEW
OF THE SLOAN
DIGITAL
SKY
, Albert
Stebbins
, Matthias Steinmetz
, Chris
Stoughton
, Michael A. Strauss ,
Stephanie
A. Snedden
depend as expected
40,90
58
26
51 on seeing and sky
10 brightness. The images
91
Mark SubbaRao
,
Yasushi
Suto
,
Alexander
S.
Szalay
,
Istv
án
Szapudi
,
Paula
Szkody
, Masayuki
Tanakaan
,
are26processed through a series12 of pipelines
that determine
The Sloan Digital
Sky Survey (SDSS; York
et al. 2000) saw
92
93
2
,
Luis
F.
A.
Teodoro
,
Aniruddha
R.
Thakar
,
Christy
A.
Tremonti
,
Douglas
L.
Tucker
,
Max
Tegmark
astrometric calibration (Pier et al. 2003) and detect and measure
first light a decade ago, with the goals of obtaining CCD imaging
94
26
43
78
E.2Vanden
Berk82,95
, S. Vidrih
, Michael
S. Vogeley
the brightnesses,
positions,
and shapes
of objects, (Lupton
in fiveAlan
broadUomoto
bands over, Daniel
10,000 deg
of high-latitude
sky,, Jan
and Vandenberg
96
9
11,97
8,98
6
al. 2001;Watters
Stoughton et, David
al. 2002).
The astrometry
is good
spectroscopy
of a ,million
and, Yogesh
100,000 Wadadekar
quasars over
Nicolegalaxies
P. Vogt
,etShannon
H. Weinberg
, Andrew
Wolfgang
Voges
22
99 seventh public data 100
26
2 the bright
milliarcseconds
(mas)
rms2per
same
region.D.With
this, its
A. this
West
, Simon
M. White
, Brian C. Wilhite release,
, AlainnatoC.45
Wonders
, Brian
Yanny
, D. coordinate
R. Yocumat
, Donald
45
12 described in more detail in 17
end, as
these goals have been
The
survey
facilities
have Zibetti
, Idit
Zehavi
, Stefano
, and Daniel B. Zucker Section 4.4. The photometry
G. realized.
York40,101
is calibrated
an20742,
AB system
also been used to carry out1 Department
a comprehensive
of Physics,imaging
Universityand
of Maryland,
College Park,toMD
USA (Oke & Gunn 1983), and the
2 Fermi
points
of the
are known to 1%–2% (Abazajian et al.
spectroscopic survey to explore
the structure,
composition,
and P.O. zero
National Accelerator
Laboratory,
Box 500,
Batavia,
ILsystem
60510, USA
Columbia
Astrophysics
Street,
New
York, NY 10027,
USA is done in two ways, by tying
2004).
The
photometric
calibration
kinematics of the Milky 3Way
Galaxy
(Sloan Laboratory,
Extension550forWest 120th
4 Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA
to
photometric
standard
stars
(Smith et al. 2002) measured by a
Galactic Understanding
and
Exploration
(SEGUE);
Yanny
et
al.
5
Space
Science
Laboratory,
Universitymore
College London,
Holmbury
Sltelescope
Mary, Surrey,
RH5
6NT,(Tucker
UK
separate
0.5
m
on
the
site
et al. 2006; Ivezić
2009), and a repeatMullard
imaging
survey
that
has
discovered
6 Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210,
USA
et
al.
2004),
and
by
using
the
overlap
between
adjacent imaging
than 500 spectroscopically confirmed
Type
Ia
supernovae
with
7 IPAC, MS
220-6, California Institute of Technology, Pasadena, CA 91125, USA
009
SEVENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY
Table 1
Coverage and Contents of DR7
Imaging
11,663 deg2
357 million unique objects
8423 deg2
2
(7646 deg in North Galactic Cap)
230 million unique objects
585 million entries (including duplicates)
3500 deg2 (more than double DR6)
3240 deg2
127 million unique objects
∼46 deg2
∼250 deg2
832 deg2
Imaging area in CAS
Imaging catalog in CAS
Legacy footprint area
Legacy imaging catalog
SEGUE footprint area, available in DASa
SEGUE footprint area, available in CAS
SEGUE imaging catalog
M31, Perseus, Sagittarius scan area
Southern Equatorial Stripe with >70 repeat scans
Commissioning (“Orion”) data
Spectroscopy
Spectroscopic footprint area
Legacy
SEGUE
Total number of plate observations (640 fibers each)
Legacy Survey plates
SEGUE and special plates
Repeat observations of plates
Total number of spectrab
Galaxies
Quasars
Stars
Sky
Unclassifiable
Spectra after removing skies and duplicates
9380 deg2
8032 deg2
1348 deg2
2564
1802
676
86
1,630,960
929,555
121,363
464,261
97,398
28,383
1,440,961
Notes.
a Includes regions of high stellar density, where the photometry is likely to be poor. See the text for details. This area also
includes some regions of overlap.
b Spectral classifications from the spectro1d code; numbers include duplicates.
data have been recalibrated using ubercalibration (Padan et al. 2008) using the overlap between adjacent scans;
ting photometry is now the default photometry found
AS. We also make available the original photometry
d by the auxiliary Photometric Telescope (Tucker et al.
he ubercalibration solution was regenerated using all
ging data, but the changes are tiny from the ubercali-
7500 deg2 . An additional dozen plates were observed to
in the nominally contiguous regions in DR6. Adding in
stripes in the Southern Galactic Cap, the Legacy spec
footprint is 8032 deg2 , a 26% increment over DR6.
In addition, spectroscopy was carried out using a
target selection algorithms designed to find stars o
variety of types as part of the SEGUE project (DR
548
ABAZAJIAN ET AL.
Vol. 182
Figure 1. Distribution on the sky of the data included in DR7 (upper panel: imaging; lower panel: spectra), shown in an Aitoff equal-area projection in J2000 Equatorial
Coordinates. The Galactic plane is the sinuous line that goes through each panel. The center of each panel is at α = 120◦ ≡ 8h , and the plots cut off at δ = −25◦ ,
below which the SDSS did not extend. The Legacy imaging survey covers the contiguous area of the Northern Galactic Cap (centered roughly at α = 200◦ , δ = 30◦ ),
as well as three stripes (each of width 2.◦ 5) in the Southern Galactic Cap. In addition, several stripes (indicated in blue in the imaging data) are auxiliary imaging data,
while the SEGUE imaging scans are indicated in red. The green scans are additional runs as described in Finkbeiner et al. (2004). In the spectroscopy panel, the lighter
regions indicate that area in the Northern Galactic Cap which is new to DR7; note that the Northern Galactic Cap is now contiguous. Red points indicate SEGUE
plates and blue points indicate other non-Legacy plates (mostly as described in the DR4 paper).
Credit: M. Blanton and the SDSS-III collaboration
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Title:
The Tenth Data
Releaseand
of the
Sloan Digital
Survey:
First Spectroscopic
Department
of Physics
Astronomy,
JohnsSky
Hopkins
University,
3400 NorthData
from theStreet,
SDSS-III
ApacheMD
Point
Observatory
Charles
Baltimore,
21218,
USA) Galactic Evolution Experiment
Authors:
Ahn,Astrophysical
Christopher P.;
Alexandroff,
Rachael;
Allende
Carlos;
Publication:
The
Journal
Supplement,
Volume
211,Prieto,
Issue 2,
article id. 17, 16 pp.
Anders,
Friedrich;
Anderson,
Scott
F.;
Anderton,
Timothy;
Andrews,
Brett H.;
(2014). (ApJS Homepage)
Aubourg, Éric; Bailey, Stephen; Bastien, Fabienne A.; Bautista, Julian E.;
Publication Date:
04/2014
Beers, Timothy C.; Beifiori, Alessandra; Bender, Chad F.; Berlind, Andreas A.;
Origin:
IOP
Beutler, Florian; Bhardwaj, Vaishali; Bird, Jonathan C.; Bizyaev, Dmitry;
Astronomy Keywords: atlases,
catalogs,
Blake, Cullen
H.;surveys
Blanton, Michael R.; Blomqvist, Michael; Bochanski, John J.;
Bolton, Adam S.; Borde, Arnaud; Bovy, Jo; Shelden Bradley, Alaina;
DOI:
10.1088/0067-0049/211/2/17
Brandt, W. N.; Brauer, Dorothée; Brinkmann, J.; Brownstein, Joel R.;
Bibliographic Code:
2014ApJS..211...17A
Busca, Nicolás G.; Carithers, William; Carlberg, Joleen K.; Carnero, Aurelio R.;
Carr, Michael A.; Chiappini, Cristina; Chojnowski, S. Drew; Chuang, Chia-Hsun;
Abstract
Comparat, Johan; Crepp,
Justin R.; Cristiani, Stefano; Croft, Rupert A. C.;
Cuesta, Antonio J.; Cunha, Katia; da Costa, Luiz N.; Dawson, Kyle S.;
The Sloan Digital Sky Survey
(SDSS)
has been
operation
since
2000 April.
This Deshpande,
paper presents
the Tenth
De Lee,
Nathan;
Dean,inJanice
D. R.;
Delubac,
Timothée;
Rohit;
Public Data Release (DR10)
fromSaurav;
its current
incarnation,
SDSS-III.
This
release includes
Dhital,
Ealet,
Anne; Ebelke,
Garrett
L.;data
Edmondson,
Edwardthe
M.;first
spectroscopic data from the
Apache Point
Observatory
Evolution
Experiment
(APOGEE), along with
Eisenstein,
Daniel
J.; Epstein,Galaxy
Courtney
R.; Escoffier,
Stephanie;
spectroscopic data from the
Baryon Massimiliano;
Oscillation Spectroscopic
Survey
through
2012 July. The
Esposito,
Evans, Michael
L.; (BOSS)
Fabbian,taken
D.; Fan,
Xiaohui;
APOGEE instrument is a near-infrared
R
~
22,500
300
fiber
spectrograph
covering
1.514-1.696
Favole, Ginevra; Femenía Castellá, Bruno; Fernández Alvar, Emma; μm. The
APOGEE survey is studying
the chemical
abundances
and radial
velocities
roughlyScott
100,000
giant star
Feuillet,
Diane; Filiz
Ak, Nurten;
Finley,
Hayley; of
Fleming,
W.; red
Fontcandidates in the bulge, bar,
disk, and
halo Frinchaboy,
of the MilkyPeter
Way.M.;
DR10
includes 178,397
of 57,454 stars,
Ribera,
Andreu;
Galbraith-Frew,
J. G.;spectra
Garcíaeach typically observed three
or more D.
times,
Derived
from these spectra
Hernández,
A.; from
GarcíaAPOGEE.
Pérez, Ana
E.; Ge,quantities
Jian; Génova-Santos,
R.; (radial
velocities, effective temperatures,
surface
andLéo;
metallicities)
also included.
Gillespie,
Brucegravities,
A.; Girardi,
Gonzálezare
Hernández,
JonayDR10
I.; also roughly
doubles the number of BOSS
spectra
over those
included
in the
NinthHong;
Data Release.
DR10
includes a total of
Gott,
J. Richard,
III; Gunn,
James
E.; Guo,
Halverson,
Samuel;
1,507,954 BOSS spectra comprising
927,844
galaxy
spectra,
182,009 quasar
159,327
Harding, Paul;
Harris,
David
W.; Hasselquist,
Sten;spectra,
Hawley,and
Suzanne
L.;stellar
spectra selected over 6373.2
deg2. Michael; Hearty, Frederick R.; Herrero Davó, Artemio; Ho, Shirley;
Hayden,
Hogg, David W.; Holtzman, Jon A.; Honscheid, Klaus; Huehnerhoff, Joseph;
Ivans, Inese
I.; Jackson,
M.; abstract
Jiang, Peng;
Jennifer Toggle
A.; Highlighting
Bibtex entry for this abstract
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formatKelly
for this
(seeJohnson,
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Kinemuchi, K.; Kirkby, David; Klaene, Mark A.; Kneib, Jean-Paul;
Koesterke, Lars; Lan, Ting-Wen; Lang, Dustin; Le Goff, Jean-Marc;
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Leauthaud,
Alexie;
Lee, Khee-Gan;
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Next Generation: LSST
• Next generation: LSST (2020 or so).
• Wide, fast, deep: 8.4m, f/1.9 primary, 9.6^2
degrees FOV, 3.2 Gpixel camera.
• 10,000 sq. degrees of sky to be covered
twice per night every 3 nights.
• Over half the sky will be visited 1000 times
over 10 years. Top ranked in Decadal
Survey.
• Design driven by four main science themes:
• Probing dark energy and dark matter.
• Inventory of the solar system.
• Exploring the transient sky.
• Mapping the Milky Way.
•
Etendue: characteristic used to determine the speed at which
a system can survey the sky to a given depth (also total
effective system throughput).
•
Etendue = Primary mirror area x FOV area
•
LSST > 300 m^2 deg^2 SDSS: 6 m^2 deg^2
•
Total LSST image volume (10 years) = 100 PB, 50 PB for the
catalog database. (1 PB = 1000 TB = 10^15 B)
•
SDSS image volume in DR7 = 16 TB.
•
Millenium simulation database = 25 TB.
•
(1 PB = 1000 TB = 10^15 B)
Intro to Databases
•
What is a Database?
•
Massive: much larger than PC memory; TB; PB
•
Data is the constant: as opposed to programs; multiple
programs operate on the same data
•
“Concurrency control”: multi-user
•
Physical data independence: operations on data are
independent from the way the data is laid out.
•
Related concept: high level, ‘declarative’, query languages (SQL)
Skills learned in this class are applicable across a wide
spectrum of jobs.