# Image Gallery

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"Any SDSS image on the SDSS Web site may be downloaded, linked to, or otherwise used for non-commercial purposes, provided that you agree to the following conditions:
You must maintain the image credits. Unless otherwise stated, images should be credited to the Sloan Digital Sky Survey.
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SDSS Images may be used in commercial publications, or for other commercial purposes, only with the explicit approval of the Astrophysical Research Consortium (ARC). Requests for such use should be directed to the ARC Corporate Office via ARC’s Business Manager."

## SN_quicklook

Screenshot of Quicklook Tool for 2011V SN from Hakobyan et al. 2012

## Cosmic_web

Provided by Peter Garnavich to represent the MaNGA Void Galaxies ancillary program.

## ytl

Picture of Yen-Ting Lin

## hsc_riz_BCG

HCS image (riz composite) of brightest cluster galaxy.

## agn

Picture of AGN MaNGA galaxy

## DwarfsMaNGA

Picture of Mariana Cano Díaz

## byler

Picture of Nell Byler

IDL TIFF file

## 7443-12703_small

Picture of 7443-12703, used for merger ancillary program.

## KRubin_pic

Picture of Kate Rubin

## letters_for_manga_e4skeb_big

Write your own message in the sky: http://writing.galaxyzoo.org/

## mangafiletypes

Example MaNGA 2d extracted spectra from different pipeline stages.

## mangaspectra

Example MaNGA central galaxy spectrum.

Typical MaNGA night sky spectrum.

MaNGA raw data

## maps_8137_12703

MaNGA bookmark of 8137-12703. Designed by Print & Design, Univ. of St Andrews.

## 7443-12703-halpha

H-alpha map of 12-193481

## 12-193481-centralspec

The central spectrum of 12-193481

## Distributing an SDSS plate to a teacher in Hawaii

Miliani Middle School Teacher, Kari Caldeira-Silva (center), collecting her SDSS plate (number 6274) at the IAU meeting in Honolulu, Hawaii from Kate Meredith (left) and Karen Masters (right)

## 7443-12703-ds9

Example ds9 display for 12-193481

## MaNGA_footprint_DR13

The MaNGA footprint as of DR13. Grey areas show all the potential regions where MaNGA may observe in the future. Blue regions show the completed plates.

## intcal_cal_giantcal

Adopted internal calibration relations for dwarfs, based on stars in clusters. Note that for some elements, no calibrated quantities have been populated, if the cluster results are very poor.

## intcal_cal_dwarfcal

Adopted internal calibration relations for dwarfs, based on stars in clusters. Note that for some elements, no calibrated quantities have been populated, if the cluster results are very poor.

## ditherpattern

Schematic diagram of the 7 central fibers within a hexagonally packed MaNGA IFU, showing the 120 micron diameter fiber core and surrounding cladding plus buffer. The triangular figure shows the relative positions of the three dither positions; the fiber bundle is located at position “S.” The central (C) “home” position
is labeled, along with the north (N), south (S), and east (E) dither positions. The nominal plate scale of the SDSS telescope is 217.7358 mm degree−1, or 60.48 microns arcsec−1

Johan Comparat

## Saurav Dhital

Research Assistant Professor – Physical Science

## temp

Comparison of ASCAP temperatures with independently derived photometric temperatures for a low-reddening sample.

## logg

Comparison of ASPCAP surface gravities with those derived from asteroseismic analysis. Blue points are stars identified by asterseismology to be core helium burning (red clump) stars.

## allfitchi2

χ2 as a function of temperature for the DR12 sample

## intcal

Internal calibration relations from cluster stars.

## MARVELS_schematic

A schematic illustration of the MARVELS spectrograph. Figure taken from Ge, Erskine, and Rushford, 2002, PASP.

## boss_twodispersive_dichroic

The assembled central optics (two dispersive elements and the dichroic).

## boss_onedispersive_dichroic

The dichroic plus one dispersive element.

## boss_beamsplitter

The dichroic (beamsplitter).

## boss_optbench

The BOSS optical bench. The large hole will hold the blue camera.

## boss_spectrograph

An illustration of the BOSS spectrograph setup

## apogee_arrival

The 2-ton APOGEE instrument is lowered to the concrete pad in front of its room in the warm building next to the telescope.

## apogee_pseudoslit

APOGEE fibers terminate in v-groove blocks. Each of the 10 v-groove blocks contain 30 fibers.

## apogee_camera

The 6-element, 250 lb, APOGEE refractive camera undergoes interferometric null-testing at New England Optical Systems, Inc.

## apogee_vph

The APOGEE mosaic Volume Phase Holographic (VPH) grating is installed during instrument assembly.

caption

## camera_filters

The SDSS-III camera filter throughput curves

## color_colorts

Example color-color diagram of SEGUE 1 target selection categories.

## stdstar_colors

The color selection of the SDSS standard stars. Red points represent stars selected as spectroscopic standards. (Most are flux standards; the very blue stars in the right hand plot are "hot standards" used for telluric absorption correction.)

## throughput

Throughput curves for the red and blue channels on the two SDSS spectrographs

## wiggle_spectrum

Figure C: The spectrum of SDSSJ172637.26+264127.6, an A0 star observed as part of SEGUE. The strong broad lines are due to Balmer absorption. The red spectrum is that available in DR6, while the black spectrum is from DR7.

## ratios

Figure B: Median flux ratios over all objects in the three exposures of plate 1916, before (left) and after (right) correction for the moving interference filters. The ratio is fit to the derivative of the interference component of the flat field (Figure A) after allowing for an arbitrary wavelength shift.

## superflat

Figure A: The decomposition of the flat field of the first blue spectrograph (upper curve) into stable (lower curve, offset slightly for clarity) and unstable (interference) components. The unstable component is close to zero, but shows wiggles at wavelengths that shift from one exposure to another.

## Sky-fpbin

Sky estimate from photo

Spline fit

Residuals

## resolve-example

Toy example of resolve, in terms of a survey with only two fields. The balkans it is broken up into are shown. The background color indicates which field is primary in which area. The RUN_PRIMARY objects for each field are shown. Except in the indicated cases, these all become SURVEY_PRIMARY in the resolve.

## resolve_balkans

Example set of balkans (polygons describing survey coverage). Note that you can see the imprint of the overlapping runs in the resulting set of disjoint polygons.

## resolve_skydist

Distribution of imaging fields on the sky. Lighter regions indicate more overlapping fields; the whitest areas have three or more overlapping fields.

## Resolve Fields

A range of fields in run 4632. Each camcol is labeled on the right, and along the top the field numbers are listed for camcol 6 (the parallel fields in the other camcols have the same field numbers).

## Figure 2: Fiber Collisions

Figure 2: Fiber Collisions

## dr1_polygons0

1. The area targeted (in dark grey) by Tile Region 4 and the boundaries of the defined tiles.

## dr1_polygons1

2. The area targeted (in dark grey) by Tile Region 5 and the boundaries of the defined tiles, plus (in lighter tones) the geometry of Tile Region 4. Note that there exist areas in Tile Region 5 which are within the boundaries of tiles from Tile Region 4; however, those old tiles could not have been assigned targets in Tile Region 5.

## dr1_polygons2

3. The area targeted (in dark grey) by Tile Region 14 and the boundaries of the defined tiles, plus (in lighter tones) the geometry of Tile Regions 4 and 5. The same issue of overlapping tiles exists in this case.

## dr1_polygons3

4. The full area covered by the targeting and all of the relevant Tile Region and tile boundaries. One can divide this region into all the disjoint polygons defined by these boundaries (for example using Andrew Hamilton's Mangle software).

## dr1_polygons4

5. One can ask for each disjoint polygon what tiles cover it. A unique set of tiles covering any area of sky is known as a "sector" or sometimes "overlap region." The last figure colors shows the same set of disjoint polygons but colors each one according to its sector. Note that sectors can consist of more than one polygon.

## Quasar target selection

Quasar target selection

## galts

The main galaxy sample target selection algorithm is detailed in Strauss et al. (2002) and is summarized here.

A third example page of QA figures for Run 94 in the r band, plotting histograms of photometric residuals for the six camera columns.

## fluxcal_94_r2

A second example page of QA figures for Run 94 in the r band, plotting photometric residuals as a function of CCD column.

## An example page of QA figures for Run 94

An example page of QA figures for Run 94 in the r band. The figure shows the mean photometric residuals as a function of field and time along the run, for the best fit photometric parameters (top panel) and correcting for overlap photometry (middle panel), with the 25%, 50% and 75% contours plotted. The bottom panel shows the number of stars used by the calibration algorithm.

caption

## faceplat2

An illustration of the arrangement of the CCDs and filters on the SDSS-III camera

## dteff_snr_best

Residual distribution of Teff as a function of S/N (click to get a larger version)

## ex_IFU_galaxy

A MaNGA target galaxy, 500 Myr away. The circles represent individual fibers in a bundle

## dr10_galaxy

Residual distribution of log g as a function of S/N (click to get a larger version).

Residual distribution of [Fe/H] as a function of S/N (click to get a larger version).

On the left, an image of the face of a 127 fiber IFU. Its ferrule housing which holds the IFU and allows it to be plugged into the SDSS plate is shown on the right.

## bgexo

Artist's conception of an extrasolar planetary system (credit: T. Riecken).

## eboss_169_v5

Previously, SDSS has mapped the universe across billions of light-years, focusing on the time from 7 billion years after the Big Bang to the present and the time from 2 billion years to 4 billion years after the Big Bang. SDSS-IV will focus on mapping the distribution of galaxies and quasars from when the universe was 3 to 8 billion years ago, a critical time when dark energy starts to affect the expansion of the Universe.
Credit: Dana Berry / SkyWorks Digital Inc. and the SDSS collaboration

## APOGEE-2

APOGEE-2 will extend the reach of the SDSS by using both the Sloan Foundation Telescope at Apache Point Observatory and the Irénée du Pont Telescope at Las Campanas Observatory in Chile.

A telescope in each hemisphere means that APOGEE-2 will be able to see the entire Milky Way. The new Chilean telescope will offer an excellent view of the galactic central regions.

Image credit: Dana Berry / SkyWorks Digital Inc. and the SDSS collaboration

## Image converted using ifftoany

The new SDSS will measure spectra at multiple points in the same galaxy, using a newly created fiber bundle.
The left-hand side shows the Sloan Foundation Telescope leading into a close-up of the tip of the fiber bundle. The bottom right illustrates how each fiber will observe a different section of the galaxy. The image from the Hubble Space Telescope shows one of the first galaxies that the new SDSS has measured. The top right shows data gathered by two fibers observing two different part of the galaxy, showing how the spectrum of the central regions differs dramatically from outer regions.
Credit: Dana Berry / SkyWorks Digital Inc., David Law, and the SDSS collaboration

asdf

## apogee_v3

The SDSS will extend its reach by using both the Sloan Foundation Telescope at Apache Point Observatory and the Irénée du Pont Telescope at Las Campanas Observatory in Chile, as shown on the left.
Because of the orientation of the Earth's axis relative to the disk of the Milky Way, the northern telescope will observe a very different part of the Milky Way (shaded in blue) than the southern telescope (shaded in green), which will have an excellent view of the galactic central regions. The survey of the Milky Way will reach different distances from the Sun, illustrated by the nested spheres, depending on survey strategy and the density of stars and dust along the line-of-sight. SDSS-IV’s gaze will also extend our neighboring dwarf galaxies, the Magellanic Clouds, shown at the bottom right.

## Image converted using ifftoany

The new SDSS will measure spectra at multiple points in the same galaxy, using a newly created fiber bundle.
The left-hand side shows the Sloan Foundation Telescope leading into a close-up of the tip of the fiber bundle. The bottom right illustrates how each fiber will observe a different section of the galaxy. The image from the Hubble Space Telescope shows one of the first galaxies that the new SDSS has measured. The top right shows data gathered by two fibers observing two different part of the galaxy, showing how the spectrum of the central regions differs dramatically from outer regions.

## eboss1c

The new SDSS will focus on mapping the distribution of galaxies and quasars 3 to 8 billion years ago, at the time when dark energy started to affect the expansion of the Universe.

## apogee1b

SDSS-IV will extend its reach by using both the Sloan Foundation Telescope and the du Pont telescope at Las Campanas Observing in Chile. Because of the orientation of the Earth’s axis relative to the disk of the Milky Way, the northern telescope sees a very different part of the Milky Way than the southern telescope, which will have an excellent view of the center of our galaxy.

CAPTION!

CAPTION!

## manga169

The new SDSS will measure spectra at multiple points in the same galaxy, using a newly created fiber bundle. The Sloan Foundation Telescope (top left) leads to a close-up of the fiber bundle tip so that each fiber can see a different part of the same galaxy (bottom right). The image from the Hubble Space Telescope (bottom right) shows one of the first galaxies the new SDSS has measured. Spectra from different parts of this galaxy (top right) show how the center of the galaxy differs from its outer regions.

## eboss1b

The new SDSS will focus on mapping the distribution of galaxies and quasars 3 to 8 billion years ago, at the time when dark energy started to affect the expansion of the Universe.

## apogee1

SDSS-IV will extend its reach by using both the Sloan Foundation Telescope and the du Pont telescope at Las Campanas Observing in Chile. Because of the orientation of the Earth’s axis relative to the disk of the Milky Way, the northern telescope sees a very different part of the Milky Way than the southern telescope, which will have an excellent view of the center of our galaxy.

## Image converted using ifftoany

The new SDSS will measure spectra at multiple points in the same galaxy, using a newly created fiber bundle.

The Sloan Foundation Telescope (top left) leads to a close-up of the fiber bundle tip so that each fiber can see a different part of the same galaxy (bottom right).

The image from the Hubble Space Telescope (bottom right) shows one of the first galaxies the new SDSS has measured. Spectra from different parts of ths galaxy (top right) show how how the center of the galaxy differs from its outer regions.

## Stacked quasar spectra

Stacked spectra of more than 46,000 quasars from the SDSS; each spectrum has been converted to a single horizontal line, and they are stacked one above the other with the closest quasars at the bottom and the most distant quasars at the top.
Credit: X. Fan and the Sloan Digital Sky Survey.

## m13

The star cluster M13 as seen by the SDSS

## IDL TIFF file

The SDSS's "Field of Streams" map shows structures of stars in the outer Milky Way

## leoi

The ultra-faint Milky Way Companion galaxy Leo I

## M51

The bright spiral galaxy M51 and its fainter companion

## Quasar wind

SDSS discovered massive changes in the wind patterns of a quasar over just nine years.

## SDSS Galaxy Map

The SDSS's map of the Universe. Each dot is a galaxy; the color bar shows the local density .

## SDSS Imaging Camera

SDSS Imaging Camera.

## segue_fields

The SEGUE-1 fields are displayed in blue and the SEGUE-2 are in red. The map is in Galactic coordinates (credit: M. Strauss).

## streams

SDSS stellar map of the Northern sky, showing trails and streams of stars torn from disrupted Milky Way satellites. Insets show new dwarf companions discovered by the SDSS (credit: V. Belokurov).

## 20120109.wander

Milky Way science: using SEGUE data with SSPP parameter estimates to determine the radial metallicity gradient of the Galactic disk (Cheng et al. 2012)

## BOSS_4382-55742-9

A randomly selected spectrum from the dr10 BOSS data, showing absorption (red) and emission (blue) lines. Click on the image to go to this object's page on SkyServer.

## BAO-DR9

Comparison of the power spectrum of SDSS-II LRGs and BOSS DR9 CMASS galaxies. Solid lines show the best-fit models. From Anderson et al. 2012.

## boss

An illustration of the concept of baryon acoustic oscillations, which are imprinted in the early universe and can still be seen today in galaxy surveys like BOSS
(Illustration courtesy of Chris Blake and Sam Moorfield).