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<title>Cosmic Origins Spectrograph</title>

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<span id="openzim-page-title" class="mw-page-title-main"><span class="mw-page-title-main">Cosmic Origins Spectrograph</span></span>

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<p>The <b>Cosmic Origins Spectrograph</b> (COS) is a science instrument that was installed on the <a href="Hubble_Space_Telescope" title="Hubble Space Telescope">Hubble Space Telescope</a> during Servicing Mission 4 (<a href="STS-125" title="STS-125">STS-125</a>) in May 2009. It is designed for <a href="Ultraviolet" title="Ultraviolet">ultraviolet</a> (90–320 nm) <a href="Spectroscopy" title="Spectroscopy">spectroscopy</a> of faint point sources with a <a href="Spectral_resolution" title="Spectral resolution">resolving power</a> of ≈1,550–24,000. Science goals include the study of the origins of large scale structure in the universe, the formation and evolution of galaxies, and the origin of stellar and planetary systems and the cold <a href="Interstellar_medium" title="Interstellar medium">interstellar medium</a>. COS was developed and built by the Center for Astrophysics and Space Astronomy (CASA-ARL) at the <a href="University_of_Colorado_at_Boulder" class="mw-redirect" title="University of Colorado at Boulder">University of Colorado at Boulder</a> and the <a href="Ball_Aerospace" class="mw-redirect" title="Ball Aerospace">Ball Aerospace and Technologies Corporation</a> in <a href="Boulder%2C_Colorado" title="Boulder, Colorado">Boulder, Colorado</a>.

</p><p>COS is installed into the axial instrument bay previously occupied by the Corrective Optics Space Telescope Axial Replacement (<a href="COSTAR" class="mw-redirect" title="COSTAR">COSTAR</a>) instrument, and is intended to complement the Space Telescope Imaging Spectrograph (<a href="STIS" class="mw-redirect" title="STIS">STIS</a>) that was repaired during the same mission. While STIS operates across a wider wavelength range, COS is many times more sensitive in the UV.<sup id="cite_ref-1" class="reference"><a href="#cite_note-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-COSHandbook_2-0" class="reference"><a href="#cite_note-COSHandbook-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup>

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<div class="mw-heading mw-heading2"><h2 id="Instrument_overview">Instrument overview</h2></div>

<p>The Cosmic Origins Spectrograph is an ultraviolet <a href="Spectrometer" title="Spectrometer">spectrograph</a> that is optimized for high sensitivity and moderate <a href="Spectral_resolution" title="Spectral resolution">spectral resolution</a> of compact (point like) objects (stars, quasars, etc.). COS has two principal channels, one for <a href="Ultraviolet#Subtypes" title="Ultraviolet">Far Ultraviolet</a> (FUV) spectroscopy covering 90–205 nm and one for <a href="Ultraviolet#Subtypes" title="Ultraviolet">Near Ultraviolet</a> (NUV) spectroscopy spanning 170–320 nm. The FUV channel can work with one of three <a href="Diffraction_grating" title="Diffraction grating">diffraction gratings</a>, the NUV with one of four, providing both low and medium resolution spectra (table 1). In addition, COS has a narrow field of view NUV imaging mode intended for target acquisition.<sup id="cite_ref-COSHandbook_2-1" class="reference"><a href="#cite_note-COSHandbook-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup>

</p><p>One key technique for achieving high sensitivity in the FUV is minimizing the number of optics. This is done because FUV reflection and transmission efficiencies are typically quite low compared to what is common at visible wavelengths. In accomplishing this, the COS FUV channel uses a single (selectable) optic to diffract the light from HST, correct for the <a href="Hubble_Space_Telescope#Flawed_mirror" title="Hubble Space Telescope">Hubble spherical aberration</a>, focus the diffracted light onto the FUV detector and correct for astigmatism typical of this sort of instrument. Since aberration correction is performed after the light passes into the instrument, the entrance to the spectrograph must be an extended aperture, rather than the traditional narrow entrance slit, in order to allow the entire aberrated HST image from a point source to enter the instrument. The 2.5 arc second diameter entrance aperture allows ≈ 95% of the light from compact sources to enter COS, yielding high sensitivity at the design resolution for compact sources.

</p>

<caption>Table 1. Principal COS Spectrographic and Target Acquisition Modes<sup id="cite_ref-COSHandbook_2-2" class="reference"><a href="#cite_note-COSHandbook-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup>

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<th>Grating (Channel)

</th>

<th>Approximate Useful <a href="Wavelength" title="Wavelength">Wavelength</a> Range

</th>

<th><a href="Spectral_resolution" title="Spectral resolution">Resolving power</a> (λ/Δλ)

</th></tr>

<tr>

<td>G130M (FUV)

</td>

<td>90–145 nm

</td>

<td>16,000–21,000

</td></tr>

<tr>

<td>G160M (FUV)

</td>

<td>141–178 nm

</td>

<td>16,000–21,000

</td></tr>

<tr>

<td>G140L (FUV)

</td>

<td><90–205 nm

</td>

<td>1,500–4,000

</td></tr>

<tr>

<td>G185M (NUV)

</td>

<td>170–210 nm

</td>

<td>22,000–28,000

</td></tr>

<tr>

<td>G225M (NUV)

</td>

<td>210–250 nm

</td>

<td>28,000–38,000

</td></tr>

<tr>

<td>G285M (NUV)

</td>

<td>250–320 nm

</td>

<td>30,000–41,000

</td></tr>

<tr>

<td>G230L (NUV)

</td>

<td>170–320 nm

</td>

<td>2,100–3,900

</td></tr>

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<td>TA1 (target acquisition imager)

</td>

<td>170–320 nm

</td>

<td>~0.05 arc sec. angular resolution

</td></tr></tbody></table>

<p>Post launch performance closely matched expectations. Instrument sensitivity is close to pre-launch calibration values, and detector background is exceptionally low (0.16 counts per resolution element per 1000 seconds for the FUV detector, and 1.7 counts per resolution element per 100 seconds for the NUV detector). FUV resolution is slightly lower than pre-launch predictions due to mid-frequency polishing errors on the HST <a href="Primary_mirror" title="Primary mirror">primary mirror</a>, while NUV resolution exceeds pre-launch values in all modes. Thanks to the minimal number of reflections, the G140L mode, and G130M central wavelength settings added after 2010, can observe light at wavelengths down to ~90 nm, and shorter, despite the very low reflectivity of the MgF<sub>2</sub> coated optics at these wavelengths.

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<div class="mw-heading mw-heading2"><h2 id="Science_goals">Science goals</h2></div>

<p>The Cosmic Origins Spectrograph is designed to enable the observation of faint, point-like UV targets at moderate spectral resolution, allowing COS to observe hot stars (<a href="OB_stars" class="mw-redirect" title="OB stars">OB stars</a>, <a href="White_dwarfs" class="mw-redirect" title="White dwarfs">white dwarfs</a>, <a href="Cataclysmic_variable_star" title="Cataclysmic variable star">cataclysmic variables</a> and <a href="Binary_star" title="Binary star">binary stars</a>) in the <a href="Milky_Way" title="Milky Way">Milky Way</a> and to observe the absorption features in the spectra of <a href="Active_galactic_nucleus" title="Active galactic nucleus">active galactic nuclei</a>. Observations are also planned of extended objects. Spectroscopy provides a wealth of information about distant astronomical objects that is unobtainable through imaging:

</p>

Spectroscopy lies at the heart of astrophysical inference. Our understanding of the origin and evolution of the cosmos critically depends on our ability to make quantitative measurements of physical parameters such as the total mass, distribution, motions, temperatures, and composition of matter in the Universe. Detailed information on all of these properties can be gleaned from high-quality spectroscopic data. For distant objects, some of these properties (e.g., motions and composition) can only be measured through spectroscopy.</p></blockquote>

<blockquote><p>Ultraviolet (UV) spectroscopy provides some of the most fundamental diagnostic data necessary for discerning the physical characteristics of planets, stars, galaxies, and interstellar and intergalactic matter. The UV offers access to spectral features that provide key diagnostic information that cannot be obtained at other wavelengths.<sup id="cite_ref-CUCOSWebpage_3-0" class="reference"><a href="#cite_note-CUCOSWebpage-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup>

</p></blockquote>

<p>Obtaining <a href="Absorption_spectra" class="mw-redirect" title="Absorption spectra">absorption spectra</a> of interstellar and intergalactic gas forms the basis of many of the COS science programs. These spectra will address questions such as how was the <a href="Cosmic_Web" class="mw-redirect" title="Cosmic Web">Cosmic Web</a> formed, how much mass can be found in interstellar and intergalactic gas, and what is the composition, distribution and temperature of this gas. In general, COS will address questions such as:<sup id="cite_ref-4" class="reference"><a href="#cite_note-4"><span class="cite-bracket">[</span>4<span class="cite-bracket">]</span></a></sup>

</p>

<ul><li>What is the large-scale structure of matter in the Universe?</li>

<li>How did <a href="Galaxies" class="mw-redirect" title="Galaxies">galaxies</a> form out of the intergalactic medium?</li>

<li>What types of <a href="Galaxy_halo" class="mw-redirect" title="Galaxy halo">galactic halos</a> and outflowing winds do <a href="Galaxy_formation" class="mw-redirect" title="Galaxy formation">star-forming galaxies</a> produce?</li>

<li>How were the chemical elements for life created in <a href="List_of_most_massive_stars" title="List of most massive stars">massive stars</a> and <a href="Supernovae" class="mw-redirect" title="Supernovae">supernovae</a>?</li>

<li>How do stars and planetary systems form from dust grains in <a href="Molecular_cloud" title="Molecular cloud">molecular clouds</a>?</li>

<li>What is the composition of <a href="Atmosphere" title="Atmosphere">planetary atmospheres</a> and <a href="Comets" class="mw-redirect" title="Comets">comets</a> in the <a href="Solar_System" title="Solar System">Solar System</a> (and beyond)?</li></ul>

<p>Some specific programs include the following:

</p><p><b>Large-Scale Structure of <a href="Baryon" title="Baryon">Baryonic Matter</a>:</b> With its high FUV spectroscopic sensitivity, COS uniquely suited for exploring the <a href="Lyman-alpha_forest" title="Lyman-alpha forest">Lyman-alpha forest</a>. This is the ‘forest’ of <a href="Absorption_spectra" class="mw-redirect" title="Absorption spectra">absorption spectra</a> seen in the spectra of distant <a href="Galaxies" class="mw-redirect" title="Galaxies">galaxies</a> and <a href="Quasars" class="mw-redirect" title="Quasars">quasars</a> caused by intergalactic gas clouds, which may contain the majority of baryonic matter in the universe. Because the most useful absorption lines for these observations are in the far ultraviolet and the sources are faint, a high sensitivity FUV spectrograph with wide wavelength coverage is needed to perform these observations. By determining the <a href="Redshift" title="Redshift">redshift</a> and line width of the intervening absorbers, COS will be able to map out the temperature, density and composition of dark <a href="Baryon" title="Baryon">baryonic matter</a> in the <a href="Cosmic_Web" class="mw-redirect" title="Cosmic Web">Cosmic Web</a>.

</p><p><b>Warm–hot <a href="Outer_space#Intergalactic_space" title="Outer space">intergalactic medium</a>:</b> Absorption line studies of highly <a href="Ionized" class="mw-redirect" title="Ionized">ionized</a> (hot) gas (<a href="Oxygen" title="Oxygen">O</a> IV, <a href="Nitrogen" title="Nitrogen">N</a> V, etc.) and broad <a href="Lyman_series" title="Lyman series">Lyman-alpha</a> will explore the ionization state and distribution of hot intergalactic gas.

</p><p><b><a href="Great_Wall_(astronomy)" class="mw-redirect" title="Great Wall (astronomy)">Great Wall</a> Structure:</b> Background <a href="Active_galactic_nuclei" class="mw-redirect" title="Active galactic nuclei">active galactic nuclei</a> will be used to study intergalactic absorbers to estimate their transverse size and physical density and determine how the distribution of material correlates with nearby galaxy distributions in the CFA2 Great Wall.

</p><p><b><a href="Reionization#Quasars_and_the_Gunn-Peterson_trough" title="Reionization">He II Reionization</a>:</b> Highly redshifted <a href="Ionized" class="mw-redirect" title="Ionized">ionized</a> helium will be used study the <a href="Reionization" title="Reionization">reionization</a> process at a <a href="Redshift" title="Redshift">redshift</a> (z) of ≈ 3.

</p>

<div class="mw-heading mw-heading2"><h2 id="Additional_instrument_design_details">Additional instrument design details</h2></div>

<p>COS has two channels, the <a href="Ultraviolet#Subtypes" title="Ultraviolet">Far Ultraviolet</a> (FUV) covering 90–205 nm and the <a href="Ultraviolet#Subtypes" title="Ultraviolet">Near Ultraviolet</a> (NUV) covering 170–320 nm. All COS optics are reflective (except for the bright object aperture filter and NUV order sorters) to maximize efficiency and to avoid <a href="Chromatic_aberration" title="Chromatic aberration">chromatic aberration</a>. Principal COS observing modes are summarized in table 1.

</p><p>Light from the Hubble Space Telescope enters the instrument through either the Primary Science Aperture (PSA) or the Bright Object Aperture (BOA). The BOA introduces a <a href="Neutral_density_filter" class="mw-redirect" title="Neutral density filter">neutral density filter</a> to the <a href="Optical_path" title="Optical path">optical path</a> that attenuates the light by approximately a factor of one hundred (five <a href="Absolute_Magnitude" class="mw-redirect" title="Absolute Magnitude">astronomical magnitudes</a>). Both apertures are oversized (2.5 arc second clear aperture) permitting more than 95% of the light from a point source to enter the <a href="Spectrograph" class="mw-redirect" title="Spectrograph">spectrograph</a>.

</p><p>After passing through the PSA or BOA the light travels to one of the optics on the first of two optic select wheels, either one of the three FUV diffraction gratings or the first of the NUV collimation mirrors (table 1), depending on whether an FUV, NUV, or target acquisition channel is selected. All optics on the first wheel have an <a href="Aspheric" class="mw-redirect" title="Aspheric">aspheric</a> profile to correct for the <a href="Hubble_Space_Telescope#Flawed_mirror" title="Hubble Space Telescope">Hubble spherical aberration</a>.

</p><p>The FUV channel has two medium and one low resolution spectroscopy modes. The FUV channels are modified Rowland Circle spectrographs in which the single <a href="Holographic_grating" title="Holographic grating">holographically ruled</a> <a href="Aspheric" class="mw-redirect" title="Aspheric">aspheric</a> <a href="Concave_mirror" class="mw-redirect" title="Concave mirror">concave</a> <a href="Diffraction_grating" title="Diffraction grating">diffraction grating</a> simultaneously focuses and diffracts the incoming light and corrects both for the HST spherical aberration and for aberrations introduced by the extreme off-Rowland layout. The diffracted light is focused onto a 170x10 mm cross delay line <a href="Microchannel_plate_detector" title="Microchannel plate detector">microchannel plate detector</a>. The FUV detector active area is curved to match the spectrograph's focal surface and is divided into two physically distinct segments separated by a small gap.

</p><p>The NUV channel has three medium and one low resolution spectroscopy modes as well as an imaging mode with an approximately 1.0 arc second unvignetted field of view. The NUV channels utilize a modified <a href="Monochromator#Czerny-Turner_monochromator" title="Monochromator">Czerny-Turner</a> design in which collimated light is fed to the selected grating, followed by three camera mirrors that direct the diffracted light onto three separate stripes on a 25×25 mm Multi Anode Microchannel Array (MAMA) detector. The imaging mode is primarily intended for target acquisition.<sup id="cite_ref-COSHandbook_2-3" class="reference"><a href="#cite_note-COSHandbook-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup>

</p>

<ul><li><a href="Advanced_Camera_for_Surveys" title="Advanced Camera for Surveys">Advanced Camera for Surveys</a></li>

<li><a href="Faint_Object_Camera" title="Faint Object Camera">Faint Object Camera</a></li>

<li><a href="Faint_Object_Spectrograph" title="Faint Object Spectrograph">Faint Object Spectrograph</a></li>

<li><a href="Goddard_High_Resolution_Spectrograph" title="Goddard High Resolution Spectrograph">Goddard High Resolution Spectrograph</a></li>

<li><a href="Near_Infrared_Camera_and_Multi-Object_Spectrometer" title="Near Infrared Camera and Multi-Object Spectrometer">Near Infrared Camera and Multi-Object Spectrometer</a></li>

<li><a href="Space_Telescope_Imaging_Spectrograph" title="Space Telescope Imaging Spectrograph">Space Telescope Imaging Spectrograph</a></li>

<li><a href="Wide_Field_and_Planetary_Camera" title="Wide Field and Planetary Camera">Wide Field and Planetary Camera</a></li>

<li><a href="Wide_Field_and_Planetary_Camera_2" title="Wide Field and Planetary Camera 2">Wide Field and Planetary Camera 2</a></li>

<li><a href="Wide_Field_Camera_3" title="Wide Field Camera 3">Wide Field Camera 3</a></li>

<li><a href="Photon_underproduction_crisis" title="Photon underproduction crisis">Photon underproduction crisis</a></li></ul>

<div class="mw-heading mw-heading2"><h2 id="References">References</h2></div>

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</style><cite class="citation web cs1"><a rel="nofollow" class="external text" href="https://web.archive.org/web/20071213072941/http://hubblesite.org/servicing_mission_4/">"HubbleSite – Servicing Mission 4"</a>. Archived from <a rel="nofollow" class="external text" href="http://hubblesite.org/servicing_mission_4/">the original</a> on 2007-12-13<span class="reference-accessdate">. Retrieved <span class="nowrap">2007-12-05</span></span>.</cite></span>

</li>

<li id="cite_note-COSHandbook-2"><span class="mw-cite-backlink">^ <a href="#cite_ref-COSHandbook_2-0"><sup><i><b>a</b></i></sup></a> <a href="#cite_ref-COSHandbook_2-1"><sup><i><b>b</b></i></sup></a> <a href="#cite_ref-COSHandbook_2-2"><sup><i><b>c</b></i></sup></a> <a href="#cite_ref-COSHandbook_2-3"><sup><i><b>d</b></i></sup></a></span> <span class="reference-text"><a rel="nofollow" class="external text" href="http://www.stsci.edu/hst/cos/documents/handbooks/current/cos_cover.html">COS Instrument Handbook</a></span>

</li>

<li id="cite_note-CUCOSWebpage-3"><span class="mw-cite-backlink"><b><a href="#cite_ref-CUCOSWebpage_3-0">^</a></b></span> <span class="reference-text"><a rel="nofollow" class="external text" href="http://cos.colorado.edu">University of Colorado COS Web Page</a></span>

</li>

<li id="cite_note-4"><span class="mw-cite-backlink"><b><a href="#cite_ref-4">^</a></b></span> <span class="reference-text"><a rel="nofollow" class="external text" href="https://arxiv.org/abs/0901.0709/">The Cosmic Origins Spectrograph and the Future of Ultraviolet Astronomy</a></span>

</li>

</ol></div></div>

<div class="mw-heading mw-heading2"><h2 id="External_links">External links</h2></div>

<ul><li><span class="noviewer" typeof="mw:File"></span> Media related to <a href="https://commons.wikimedia.org/wiki/Category:Cosmic_Origins_Spectrograph" class="extiw external" title="commons:Category:Cosmic Origins Spectrograph">Cosmic Origins Spectrograph</a> at Wikimedia Commons</li>

<li>The <a rel="nofollow" class="external text" href="http://cos.colorado.edu">Cosmic Origins Spectrograph Web Site</a> at the <a href="University_of_Colorado%2C_Boulder" class="mw-redirect" title="University of Colorado, Boulder">University of Colorado</a></li>

<li>the <a rel="nofollow" class="external text" href="http://www.stsci.edu/hst/cos">COS Web site</a> at the <a rel="nofollow" class="external text" href="http://www.stsci.edu">Space Telescope Science Institute</a> (STScI)</li></ul>

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</style><div id="Hubble_Space_Telescope391" style="font-size:114%;margin:0 4em"><a href="Hubble_Space_Telescope" title="Hubble Space Telescope">Hubble Space Telescope</a></div></th></tr><tr><th scope="row" class="navbox-group" style="width:1%">Current instruments</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em">

<ul><li><a href="Advanced_Camera_for_Surveys" title="Advanced Camera for Surveys">Advanced Camera for Surveys (ACS)</a></li>

<li><a href="Fine_Guidance_Sensor_(HST)" title="Fine Guidance Sensor (HST)">Fine Guidance Sensor (FGS)</a></li>

<li><a href="Near_Infrared_Camera_and_Multi-Object_Spectrometer" title="Near Infrared Camera and Multi-Object Spectrometer">Near Infrared Camera and Multi-Object Spectrometer (NICMOS)</a></li>

<li><a href="Space_Telescope_Imaging_Spectrograph" title="Space Telescope Imaging Spectrograph">Space Telescope Imaging Spectrograph (STIS)</a></li>

<li><a href="Wide_Field_Camera_3" title="Wide Field Camera 3">Wide Field Camera 3 (WFC3)</a></li></ul>

</div></td><td class="noviewer navbox-image" rowspan="5" style="width:1px;padding:0 0 0 2px"><div><span typeof="mw:File"></span><br><span typeof="mw:File"></span></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Previous instruments</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em">

<ul><li><a href="Corrective_Optics_Space_Telescope_Axial_Replacement" title="Corrective Optics Space Telescope Axial Replacement">Corrective Optics Space Telescope Axial Replacement (COSTAR)</a></li>

<li><a href="Faint_Object_Camera" title="Faint Object Camera">Faint Object Camera (FOC)</a></li>

<li><a href="Faint_Object_Spectrograph" title="Faint Object Spectrograph">Faint Object Spectrograph (FOS)</a></li>

<li><a href="Goddard_High_Resolution_Spectrograph" title="Goddard High Resolution Spectrograph">Goddard High Resolution Spectrograph (GHRS/HRS)</a></li>

<li><a href="High_Speed_Photometer" title="High Speed Photometer">High Speed Photometer (HSP)</a></li>

<li><a href="Wide_Field_and_Planetary_Camera" title="Wide Field and Planetary Camera">Wide Field and Planetary Camera (WFPC)</a></li>

<li><a href="Wide_Field_and_Planetary_Camera_2" title="Wide Field and Planetary Camera 2">Wide Field and Planetary Camera 2 (WFPC2)</a></li></ul>

</div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="Space_Shuttle" title="Space Shuttle">Space Shuttle</a> missions</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em">

<ul><li><i>Launch:</i> <a href="STS-31" title="STS-31">STS-31</a> <small>(1990, <a href="Space_Shuttle_Discovery" title="Space Shuttle Discovery"><i>Discovery</i></a>)</small></li>

<li><i>Servicing:</i> <a href="STS-61" title="STS-61">STS-61</a> <small>(1993, <a href="Space_Shuttle_Endeavour" title="Space Shuttle Endeavour"><i>Endeavour</i></a>)</small></li>

<li><a href="STS-82" title="STS-82">STS-82</a> <small>(1997, <i>Discovery</i>)</small></li>

<li><a href="STS-103" title="STS-103">STS-103</a> <small>(1999, <i>Discovery</i>)</small></li>

<li><a href="STS-109" title="STS-109">STS-109</a> <small>(2002, <a href="Space_Shuttle_Columbia" title="Space Shuttle Columbia"><i>Columbia</i></a>)</small></li>

<li><a href="STS-125" title="STS-125">STS-125</a> <small>(2009, <a href="Space_Shuttle_Atlantis" title="Space Shuttle Atlantis"><i>Atlantis</i></a>)</small></li></ul>

</div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Special fields<br>and images</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em">

<ul><li><i><a href="Pillars_of_Creation" title="Pillars of Creation">Pillars of Creation</a></i> <small>(1995)</small></li>

<li><a href="Hubble_Deep_Field" title="Hubble Deep Field">Hubble Deep Field</a> <small>(1995)</small></li>

<li><a href="Hubble_Deep_Field_South" title="Hubble Deep Field South">Hubble Deep Field South</a> <small>(1998)</small></li>

<li><a href="Hubble_Ultra-Deep_Field" title="Hubble Ultra-Deep Field">Hubble Ultra-Deep Field</a> <small>(2003–04)</small></li>

<li><a href="Extended_Groth_Strip" title="Extended Groth Strip">Extended Groth Strip</a> <small>(2004–05)</small></li>

<li><a href="Sagittarius_Window_Eclipsing_Extrasolar_Planet_Search" title="Sagittarius Window Eclipsing Extrasolar Planet Search">SWEEPS</a> <small>(2006)</small></li>

<li><i><a href="Mystic_Mountain" title="Mystic Mountain">Mystic Mountain</a></i> <small>(2010)</small></li>

<li><a href="Hubble_eXtreme_Deep_Field" class="mw-redirect" title="Hubble eXtreme Deep Field">Hubble eXtreme Deep Field</a> <small>(2012)</small></li>

<li><i><a href="Zooming_In_on_the_Andromeda_Galaxy" title="Zooming In on the Andromeda Galaxy">Zooming In on the Andromeda Galaxy</a></i> <small>(2015)</small></li>

<li><a href="Hubble_Legacy_Field" title="Hubble Legacy Field">Hubble Legacy Field</a> <small>(2019)</small></li>

<li><a href="Great_Observatories_Origins_Deep_Survey" title="Great Observatories Origins Deep Survey">Great Observatories Origins Deep Survey</a></li>

<li><a href="List_of_Hubble_Space_Telescope_anniversary_images" title="List of Hubble Space Telescope anniversary images">Anniversary images</a></li>

<li><a href="List_of_deep_fields" title="List of deep fields">List of deep fields</a></li></ul>

</div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Related</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em">

<ul><li><a href="Great_Observatories_program" title="Great Observatories program">Great Observatories program</a></li>

<li><a href="Space_Telescope_Science_Institute" title="Space Telescope Science Institute">Space Telescope Science Institute</a></li>

<li><a href="Goddard_Space_Flight_Center" title="Goddard Space Flight Center">Goddard Space Flight Center</a></li>

<li><a href="Edwin_Hubble" title="Edwin Hubble">Edwin Hubble</a></li>

<li><i><a href="Hubble_(film)" title="Hubble (film)">Hubble</a></i> (2010 documentary)</li>

<li><a href="Hubble_Origins_Probe" title="Hubble Origins Probe">Hubble Origins Probe</a></li></ul>

</div></td></tr><tr><td class="navbox-abovebelow" colspan="3"><div>

<ul><li><span class="noviewer" typeof="mw:File"><span title="Category"></span></span> <b>Category</b></li>

<li><span class="noviewer" typeof="mw:File"><span title="Commons page"></span></span> <a href="https://commons.wikimedia.org/wiki/Category:Hubble_Space_Telescope" class="extiw external" title="commons:Category:Hubble Space Telescope"><b>Commons</b></a></li></ul>

</div></td></tr></tbody></table></div></div><div><div class="zim-footer">

This article is issued from <a class="external text" title="Last edited on 2025-06-21" href="https://en.wikipedia.org/wiki/?title=Cosmic_Origins_Spectrograph&oldid=1296661760">Wikipedia</a>. The text is available under <a class="external text" href="https://creativecommons.org/licenses/by-sa/4.0/deed.en">Creative Commons Attribution-Share Alike 4.0</a> unless otherwise noted. Additional terms may apply for the media files.

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