Gemini Observatory
https://www.gemini.edu
enIntegration Time Calculator
https://www.gemini.edu/instrumentation/texes/integration-time-calculator
<h2>Integration Time Calculator</h2><h2>Integration Time Calculator</h2>
<h3>Integration Time Calculator Table</h3>
<p><a href="https://docs.google.com/spreadsheets/d/1dZERDL27AubJEc_6o-C2C1zIsGLQgqj4/edit?usp=drive_link&ouid=109733496396045042823&rtpof=true&sd=true" target="_blank">Integration Time Calculator Table</a></p>
<h3>Timecalc.xlsx user instructions.</h3>
<p>To run the excel spreadsheet timecalc.xlsx either: <strong>1)</strong> Download and run it on your local machine using whatever system you have available, or <strong>2)</strong> open it in Google Sheets, go to <strong>File > Save as Google Sheets</strong> to make your own (writeable) copy and then use that one.</p>
<p>To calculate the time required to achieve a given SNR in nod mode, parameters are put into the white boxes in one of the columns of the Object parameters section of the Sample page of timecalc. The first 9 columns have been filled in with sample numbers. They can be overwritten or turned off by changing the on-source times to 0. When the white boxes are filled in, timecalc will calculate the values in the shaded boxes. The SNR box is most relevant. Generally the user will change the on-source time to get the desired SNR. If ‘new setup?’ or ‘new acquisition?’ are set to 1 overhead time will be added to the total time.</p>
<p>To calculate the time required for a scan-mode observation fill in the scan parameters white boxes. The on-source time and scan motion factor will be calculated, to be entered into the boxes above to calculate the SNR in the scan after binning by ‘points binned’.</p>
<p>Total times for the project are given in the shaded boxes at the left (assuming the on-source time, new acquisition, and new setup boxes in unused Object parameter columns are set to 0).</p>
<p>If fluxes are known in units other than Jy they can be converted to Jy by using the Unit Conversion page of timecalc, by filling in the white boxes of the section of the table for the conversion desired.</p>
<div class="label-above">Instrument</div>TEXESWed, 27 Mar 2024 18:41:13 +0000Fabian Bejarano22362 at https://www.gemini.eduhttps://www.gemini.edu/instrumentation/texes/integration-time-calculator#commentsSensitivity and Time Requests
https://www.gemini.edu/instrumentation/texes/sensitivity-and-time-requests
<h2>Sensitivity and Time Requests</h2><h2>Sensitivity and Time Requests</h2>
<p>In most modes TEXES is background photon noise limited. Since the background brightness and the array efficiency vary considerably with wavelength it can be difficult to calculate the instrument sensitivity at specific wavelengths, but some general rules can be given. For more precise predictions proposers may be able to use the ITC timecalc.xlsx or are encouraged to contact TEXES team members (lacy@astro.as.utexas.edu and tgreathouse@swri.edu). (To use the ITC fill in the white rows of the Object Parameters section. The colored rows will be calculated.)</p>
<p>For observers who have observed their objects with TEXES on the IRTF or on previous Gemini runs it is best to scale from the performance there. For observations of point sources the sensitivity improves in proportion to the telescope area, or a factor of 7 going to Gemini from the IRTF. For extended sources the surface brightness sensitivity is unchanged, but the spatial resolution improves in proportion to the telescope diameter, or a factor or 8/3 and the instantaneous solid angle coverage decreases by a factor of (8/3)^2.</p>
<p>For observers who cannot scale from IRTF observations the variation in NEFD in hi-med and hi-low modes caused by the instrument response and telescope background can be approximated by NEFD[in Jy, 1 sigma in 1 sec on-source, averaged over 1 spectral resolution element (2 pixels * (lambda/10um) longward of 11um, and 3 pixels shortward), and optimally extracted from the echellogram] = lambda(in micrometers)/7. To get the noise in the observed spectrum after correction for telluric transmission one needs to multiply by [(0.07 + telluric emissivity)/0.07]^0.5/(telluric transmission). This calculation may require a high-resolution telluric model, which can be obtained from the TEXES team. There are two additional factors to consider. First, the sensitivity degrades toward the ends of echelon spectral orders and at wavelengths longward of 11um the ends of orders fall off of the array and are not observed; for complete spectral coverage two settings may be required. And second, if the slit is too short to allow nodding a source along the slit, which most often occurs at short wavelengths and in hi-low mode, the telescope must nod onto blank sky, increasing the observing time by a factor of 2.</p>
<p>In med and low resolution modes the NEFD should in principle improve in proportion to the square root of the resolution width, or by factors of approximately 2.2 and 5 respectively, but in practice telluric division and array performance are typically worse in these modes so the improvements are typically not this large. It should be noted that the spectral coverage in med mode is the same as it is in hi-med, and a hi-med spectrum can be binned down to med resolution giving approximately the same NEFD as if originally observed in med mode. The main advantages of med mode for observations of moderately broad spectral features are that there is no fall-off in the sensitivity toward the ends of hi-res orders or gaps between observed orders, and that the slit is much longer for mapping observations.</p>
<p>For observations of extended sources the surface brightness sensitivity, or NESB, can be calculated from the above formulas assuming the beam to be diffraction limited. The diffraction-limited beam size is 0.028"*lambda(um), which is approximately 2 pixels along the slit at 10um. Extended sources are often observed in a mapping observing mode so to calculate the observing time one must multiply by the number of steps in the map. Typically, sources are mapped by stepping over a distance somewhat greater than the object width and using measurements off of the ends of the scan to sample the sky. In this case it is not necessary to nod the telescope at each point in the map, improving the observing efficiency. This observing mode is referred to as scan mode. Typically, the telescope step size in a scan is about half the slit width in a direction perpendicular to the slit length.</p>
<p>To calculate the total time for a project one must include overhead for spectral setup, source acquisition, delay time each time the telescope is nodded either along the slit or onto blank sky, and flat field measurement. Proposers should include in their time requests the following: 1) 5 min for each change in spectral setup, 2) 10 min to acquire a new source, 3) 33% of the on-source time for delays after telescope nods, and 4) 16% of the on-source time for flats. Under good sky conditions the last two factors can be decreased by nodding less often and including more nod pairs in a file, but it is best to use these factors in the time request. Scan-mode observations involve less overhead as there is no delay between scan steps, eliminating overhead 3 and setting overhead 4 to 1 min per file, but adding a scan setup time of 5 min. If comparison sources are used their observing and overhead times must also be included in the time request, but we have found that division by a telluric model (which can be done by the TEXES team in the data reduction) produces as good of results as division by a comparison source. The exception to this might be for observations of spectral features substantially broader than the spectral resolution, which can be affected by fringing.</p>
<p>We should note that for scan-mode observations of planets it is not unusual for the objects to be bright enough that the time per step to be limited by observing efficiency rather than S/N (and the argument for using Gemini is to achieve higher spatial resolution the can be achieved on the IRTF, rather than higher sensitivity). In this case the time between steps should be set to 2 sec, or perhaps longer on faint and small sources.</p>
<h3>Telluric Transmission at TEXES high resolution</h3>
<p><a href="https://drive.google.com/file/d/1jG5Y-okMqtX_Y9OQkMxf21auh_ruBBZp/view" target="_blank">Telluric Transmission at TEXES high resolution</a></p>
<div class="label-above">Instrument</div>TEXESFri, 22 Mar 2024 22:34:15 +0000iromero22361 at https://www.gemini.eduhttps://www.gemini.edu/instrumentation/texes/sensitivity-and-time-requests#commentsAvoid updating to Sonoma 14.4
https://www.gemini.edu/news/general-announcements/avoid-updating-sonoma-144
<p>We strongly advise Mac users running on Apple silicon systems to refrain from updating their operating system to Sonoma 14.4 until further notice.<br />
Updating to this version may result in disruptions to the functionality of our <a href="https://www.gemini.edu/observing/phase-ii/ot">Observing Tool (OT)</a>, <a href="https://www.gemini.edu/observing/phase-i/pit">Phase I Tool (PIT)</a>, and other Java based tools.</p>
<p>"An issue introduced by macOS 14.4, which causes Java process to terminate unexpectedly, is affecting all Java versions from Java 8 to the early access builds of JDK 22. There is no workaround available, and since there is no easy way to revert a macOS update, affected users might be unable to return to a stable configuration unless they have a complete backup of their systems prior to the OS update."<br />
See <a href="https://blogs.oracle.com/java/post/java-on-macos-14-4">source</a> for more information.</p>
<p></p>
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</section>Thu, 21 Mar 2024 16:19:14 +0000Aleksandar Cikota22352 at https://www.gemini.eduhttps://www.gemini.edu/news/general-announcements/avoid-updating-sonoma-144#commentsGNIRS LR- and HR-IFU released for science use
https://www.gemini.edu/news/instrument-announcements/gnirs-lr-and-hr-ifu-released-science-use
<p text-align:="justify">As part of the <a href="https://www.gemini.edu/instrumentation/instrumentation/instrument-upgrade-program">Gemini Instrument Upgrade Program</a> GNIRS has gained two new optical sub-systems, namely the LR-IFU and the HR-IFU. The commissioning of both IFUs has now been completed. The LR-IFU is available for observations in both regular queue and <a href="https://www.gemini.edu/observing/phase-i/ft/ft-cfp">Fast Turnaround</a> and the HR-IFU is offered in shared-risk in the <a href="https://www.gemini.edu/observing/phase-i/standard-semester-program/2024b-call-proposals">2024B Call for proposal</a> and will be released for Fast Turnaround at a later date.</p>
<p text-align:="justify">Raw data collected during the commissioning of the two IFUs are publicly available on the Gemini archive under the program <a href="https://archive.gemini.edu/searchform/cols=CTOWBEQ/GN-2022A-ENG-132/not_site_monitoring/GNIRS/includeengineering/science/NotFail">GN-2022A-ENG-132</a>. Note that the Gemini IRAF package update to support the reduction of GNIRS IFU data is in preparation and will be released in the near future.</p>
<div class="label-above">Tags</div><a href="/tags/gnirs" typeof="skos:Concept" property="rdfs:label skos:prefLabel" datatype="">GNIRS</a><div class="label-above">News Category</div><a href="/news/instrument-announcements" typeof="skos:Concept" property="rdfs:label skos:prefLabel" datatype="">Instrument Announcements</a><section class="block block-block block-block-2--2 ">
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</section>Wed, 13 Mar 2024 21:23:13 +0000emanuele.farina22351 at https://www.gemini.eduhttps://www.gemini.edu/news/instrument-announcements/gnirs-lr-and-hr-ifu-released-science-use#commentsMarch 2024 Call for Proposals
https://www.gemini.edu/news/fast-turnaround-call-proposals/march-2024-call-proposals
<p><strong>Gemini North and South are accepting proposals for the Fast Turnaround (FT) program in this call.</strong> Here, we give information specific to this proposal cycle. Please see the other FT pages - particularly the <a href="/observing/phase-i/FT#Rules">rules</a> - for general information about the program. <strong>FT (dual anonymous)-specific proposal <a href="https://noirlab.edu/science/node/46666">templates</a> (GemPhaseI_FT_dual) must </strong><strong>now</strong><strong> be used for all FT proposals.</strong><strong> </strong>See the "PIT information" section below.<strong> The <a href="https://noirlab.edu/science/node/46666">2024A PIT</a> must be used.</strong></p>
<p><strong>Important dates</strong></p>
<ul>
<li>
<h3>Proposal deadline: <strong>12:00pm (NOON), Hawaiian Standard Time (HST), March 31.</strong></h3>
</li>
<li>Please ensure the latest version of the PIT is used for submission (see the PIT information below).</li>
<li>Reviews must be completed by 23:59 HST, April 14. If you have submitted a proposal, but by the 2nd of the month have not received an email from FT regarding reviewing proposals, contact FT as soon as possible.</li>
<li>Results will be announced by April 21, 2024.</li>
<li>The deadline for preparing observations (Phase II) is April 30. Accepted programs meeting this deadline will be active from 1 May until 31 July 2024.</li>
<li>FT observations will be merged with the queue and observed on queue nights.</li>
</ul>
<p><strong>Dual Anonymous Review Process (DARP)</strong></p>
<ul>
<li>Since Feb 2021, we have been using a dual anonymous review process. New proposal templates for FT have been updated. <strong>DARP compliance is mandatory. Proposals using the wrong template will be removed from consideration. Proposals that do not follow all the DARP guidelines will either be removed from consideration or sent to the directorate for review. </strong></li>
<li>Guideline for PIs
<ul>
<li>Enter information of the proposing team with the Phase I Tool (PIT) as usual.</li>
<li>Use the FT specific template.</li>
<li>The proposal <a href="https://noirlab.edu/science/node/46666">template</a> has been updated to be compliant with DARP since Feb 1, 2021</li>
<li>Avoid mentioning names and affiliations of the team in the PDF attachment that could be used to identify the proposing team.</li>
<li>Avoid claiming ownership of past work. (E.g., “my successful Gemini program in the previous semester (GS-18A-xxx)”, or “our analysis shown in Doe et al. 2020…”)</li>
<li>Including text in proposals discussing previous use of Gemini is ok, as long as that work is not referenced and program IDs are not listed.</li>
<li>Cite references in passive third person, e.g., “Analysis shown in Doe et al. 2020”, including references to data and software.</li>
<li>Do describe the proposed work, e.g., “We propose to do the following…”, or “We will measure the effects of …”</li>
<li>Unpublished work can be referred to as “obtained in private communication” or “from private consultation”.</li>
</ul>
</li>
<li>Guideline for Reviewers
<ul>
<li>Accept the assigned proposals based on abstracts whether you can provide an unbiased review or not.</li>
<li>Review proposals solely based on the scientific merit of what is proposed.</li>
<li>Do not spend any time attempting to identify the PI or the team. Even if you think you know, you can be wrong.</li>
<li>Utilize neutral pronouns (they/the PI/the team) when you write comments.</li>
<li><strong>Flag the proposals that have not been sufficiently anonymized but DO NOT penalize them by lowering grades. </strong>(The FT support team will check the flagged proposals and send any violations to the Gemini Directorate for review.) </li>
</ul>
</li>
<li>More detailed guidelines can be found on the <a href="/observing/phase-i/ft#Dual%20Anonymous%20Review%20Process">FT webpage</a>. </li>
</ul>
<p><strong>Eligibility</strong></p>
<ul>
<li>PIs from all participant countries (except Chile) taking part in the FT program may apply for this cycle.</li>
<li>PIs from UH are able to apply for FT time at GS as US, but may not apply for GN time. </li>
<li>Chile and UH have withdrawn from Fast Turnaround since 2021A and 2024A, respectively.</li>
<li>In agreement with Subaru Observatory, Japanese community proposers may only apply for up to 4 hrs of time on a single proposal (and no more than 4hrs total will be awarded to Japanese community PIs in a cycle). </li>
<li>PIs from participant countries whose FT time for the semester has been used up should not apply for the remainder of the semester. At this time, <strong>KR has used its full allocation</strong> and KR users should not apply for the remainder of 24A. Note that some participant countries only have very small amounts of FT time available each semester. AR has only 2.2h and 1.8h available for this cycle at GN and GS, respectively. See <a href="/observing/phase-i/FT#Rules">Rule #4</a> and <a href="http://gemini.edu/observing/phase-i/FT#FAQ">Q&A</a> for more information.</li>
</ul>
<p><strong>Acceptable RA ranges</strong></p>
<ul>
<li><strong>Gemini North: </strong>Targets from about RA = 8.5 hr to 2.5 hr are acceptable during this cycle. Note, however, that RAs near 8.5h will only be accessible for a couple hours during the first half of the first month (May) and only at northern declinations (Dec > 0) . Likewise, RAs near 2.5h will only be accessible for a couple hours during the final month (July) and again only in the above declination range. Note <a href="/observing/phase-i/FT#Rules">Rule #9</a>; an FT program may not fully backload its three-month active period; at least one of its targets must be observable during its first active month.</li>
<li>
<p><strong>Gemini South:</strong> Targets from about RA = 7.5 hr to 3.5 hr are acceptable during this cycle. Note that RAs near 7.5h will only be accessible for a couple hours during the first half of the first month (May) and only at favorable declinations (Dec< 0) . Likewise, RAs near 3.5h will only be accessible for a couple hours during the final month (July) and again only in the above declination range. Note <a href="/observing/phase-i/FT#Rules">Rule #9</a>; an FT program may not fully backload its three-month active period; at least one of its targets must be observable during its first active month.</p>
</li>
</ul>
<p><strong>Available instruments and observing modes</strong></p>
<p><strong>Gemini North</strong></p>
<ul>
<li>GMOS-N, GNIRS, and MAROON-X are available throughout much of the cycle. </li>
<li>We are offering Altair in NGS mode only, with GNIRS.</li>
<li>The <strong>GNIRS Low-Resolution IFU</strong> is offered. However, be aware that the Gemini IRAF package for the LR-IFU is in preparation and will not be released until sometime in May 2024. In the interim, PIs who receive FT data may request a patch package, which is made available on a best-effort basis only; bugs will not be fixed before the May release.</li>
<li>LGS is <strong>not</strong> currently offered this cycle. </li>
<li>Alopeke is available during a single block in May. If observations are needed outside of Alopeke blocks, please contact the FT team before proposal submission to check for additional availability.</li>
<li>Make sure to check the <a href="/sciops/metrics/gn2024Aoverview.html">24A schedule </a>for detailed instrument availability.</li>
<li>For MAROON-X, it is now possible to check for target duplications. Please see the instructions in the <a href="https://www.gemini.edu/instrumentation/maroon-x/proposal-preparation">Phase I checklist</a>.</li>
<li>Please contact the FT team in advance with any specific questions (Fast.Turnaround at gemini.edu).</li>
</ul>
<p><strong>Gemini South</strong></p>
<ul>
<li><strong>GHOST</strong> is offered this cycle.</li>
<li>GMOS-S and F2 are also available this cycle. Note that data reduction software for GMOS-S (with new CCDs) will likely not be available until mid-2024. </li>
<li>F2 MOS is <strong>not offered</strong> in this cycle. F2 MOS is limited by the number of masks that can be inserted in the instrument and will likely again be offered for the June-August FT cycle.<!-- Please read about its capabilities carefully. Since pre-images will be needed for most programs, F2 MOS targets are further restricted between RA 8 hr and 20 hr in this cycle. Please contact the Fast Turnaround team before submission if you believe you will not need pre-imaging. A maximum of 8 masks can be installed in the instrument. --></li>
<li>IGRINS is no longer offered. </li>
<li>Zorro is available for a single block in July. If you require Zorro observations outside of Zorro blocks, please check for availability with the FT team ahead of proposal submission. </li>
<li>Please check the instrument's schedule or contact the FT team in advance with any specific questions (Fast.Turnaround at gemini.edu). </li>
<li>Make sure to check the <a href="/sciops/metrics/gs2024Aoverview.html">24A instrument schedule</a> for detailed instrument availability.</li>
<li>GeMS/GSAOI are not offered via FT.</li>
</ul>
<p><strong>Both telescopes</strong></p>
<ul>
<li>FT observations may not be executed during classical observing, or priority visitor (PV), depending on the prevailing conditions.</li>
<li>For visiting instruments not listed above, please contact the FT team to check availability (Fast.Turnaround at gemini.edu).</li>
<li>The R600 grating in each GMOS instrument is NOT offered for FT (or regular queue) observations.</li>
<li>MOS observations are available for FT, subject to some caveats/restrictions.</li>
<li>As discussed in the <a href="/observing/phase-i/FT#Rules">rules</a> and <a href="http://gemini.edu/observing/phase-i/FT#FAQ">Q&A</a>, please contact the Fast Turnaround team in advance of the deadline if you would like to propose for an unusual instrument configuration or observing mode.</li>
</ul>
<p><strong>Time available</strong></p>
<ul>
<li>At this point, no partners have used up their <a href="/observing/phase-i/FT#Rules">FT shares</a>. </li>
<li>Up to 17.7 (14.7) hrs per cycle at GN (GS) is available for FT observations. Very roughly, this implies:
<ul>
<li>4 (3) hrs of 20%-ile conditions (IQ=20, for example; see <a href="/observing/telescopes-and-sites/sites#Constraints">this web page</a>)</li>
<li>9 (7.4) hrs of 50%-ile conditions</li>
<li>12.4 (10.3) hrs of 70%-ile conditions</li>
<li>15 (12.5) hrs of 85%-ile conditions</li>
</ul>
</li>
<li>PIs may propose for up to the amount of time in their most restrictive observing conditions, subject to <a href="/observing/phase-i/FT#Rules">partner's time availability - see rule #4</a>. For example, a proposal requesting CC50 IQ20 SB50 WVany conditions can request no more than 4 hrs of observing time.</li>
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</section>Sat, 02 Mar 2024 02:39:47 +0000kchiboucas22350 at https://www.gemini.eduhttps://www.gemini.edu/news/fast-turnaround-call-proposals/march-2024-call-proposals#comments2024B Call for Proposals Released
https://www.gemini.edu/news/general-announcements/2024b-call-proposals-released
<p>The <a href="/observing/phase-i/standard-semester-program/2024b-call-proposals">2024B Gemini Observatory Call for Proposals</a> has been released. Proposals are being accepted for observations from 1 August, 2024 to 31 January, 2025. Gemini North and Gemini South are expected to have 153 and 157 nights available for science, respectively. A new version of the Phase I Tool (<a href="/observing/phase-i/pit">PIT</a>) has been released to support proposal submissions. Please note that all Gemini proposals requesting time from the United States, Canada, Brazil or Argentina must be anonymized. This applies to programs requesting time only from each of those partners, and to joint programs requesting time from multiple participants which include them. The submission deadline ranges from 31 March to 3 April, 2024 as outlined <a href="/observing/phase-i/standard-semester-program/2024b-call-proposals">here</a>.</p>
<p>For more information about Gemini’s capabilities see the <a href="https://noirlab.edu/public/media/archives/brochures/pdf/brochure001.pdf">Capabilities brochure</a>.</p>
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</section>Thu, 29 Feb 2024 21:32:54 +0000mark.rawlings22349 at https://www.gemini.eduhttps://www.gemini.edu/news/general-announcements/2024b-call-proposals-released#commentsAstronomers Measure Heaviest Black Hole Pair Ever Found
https://www.gemini.edu/pr/astronomers-measure-heaviest-black-hole-pair-ever-found
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<p><a href="/es/astron-mos-miden-el-par-de-agujeros-negros-m-s-pesado-jam-s-encontrado">En Español</a></p>
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<p><em><strong>Data from Gemini North provide possible explanation for supermassive binary black hole’s halted merger</strong></em></p>
<p><strong>Using archival data from the Gemini North telescope, a team of astronomers have measured the heaviest pair of supermassive black holes ever found. The merging of two supermassive black holes is a phenomenon that has long been predicted, though never observed. This massive pair gives clues as to why such an event seems so unlikely in the Universe.</strong></p>
<p>Nearly every massive galaxy hosts a <a href="https://en.wikipedia.org/wiki/Supermassive_black_hole">supermassive black hole</a> at its center. When two galaxies merge, their black holes can form a binary pair, meaning they are in a bound orbit with one another. It’s hypothesized that these binaries are fated to eventually merge, but this has never been observed [1]. The question of whether such an event is possible has been a topic of discussion amongst astronomers for decades. In a recently published paper in <em>The Astrophysical Journal</em>, a team of astronomers have presented new insight into this question.</p>
<p>The team used data from the <a href="https://noirlab.edu/public/programs/gemini-observatory/gemini-north/">Gemini North telescope</a> in Hawai‘i, one half of the <a href="http://gemini.edu">International Gemini Observatory</a> operated by NSF’s NOIRLab, which is funded by the U.S. National Science Foundation, to analyze a supermassive black hole binary located within the elliptical galaxy <a href="https://en.wikipedia.org/wiki/4C_%2B37.11">B2 0402+379</a>. This is the only supermassive black hole binary ever resolved in enough detail to see both objects separately [2], and it holds the record for having the smallest separation ever directly measured — a mere 24 light-years [3]. While this close separation foretells a powerful merger, further study revealed that the pair has been stalled at this distance for over three billion years, begging the question; what’s the hold-up?</p>
<p>To better understand the dynamics of this system and its halted merger the team looked to archival data from Gemini North’s Gemini Multi-Object Spectrograph (<a href="https://www.gemini.edu/instrumentation/gmos">GMOS</a>), which allowed them to determine the speed of the stars within the vicinity of the black holes. <em>“The excellent sensitivity of GMOS allowed us to map the stars’ increasing velocities as one looks closer to the galaxy’s center,”</em> said Roger Romani, Stanford University physics professor and co-author of the paper. <em>“With that, we were able to infer the total mass of the black holes residing there.”</em></p>
<p>The team estimates the binary’s mass to be a whopping 28 billion times that of the Sun, qualifying the pair as the heaviest binary black hole ever measured. Not only does this measurement give valuable context to the formation of the binary system and the history of its host galaxy, but it supports the long-standing theory that the mass of a supermassive binary black hole plays a key role in stalling a potential merger [4].</p>
<p><em>“The data archive serving the International Gemini Observatory holds a gold mine of untapped scientific discovery,"</em> says Martin Still, NSF program director for the International Gemini Observatory. <em>"Mass measurements for this extreme supermassive binary black hole are an awe-inspiring example of the potential impact from new research that explores that rich archive.”</em></p>
<p>Understanding how this binary formed can help predict if and when it will merge — and a handful of clues point to the pair forming via multiple <a href="https://en.wikipedia.org/wiki/Galaxy_merger">galaxy mergers</a>. The first is that <a href="http://simbad.u-strasbg.fr/simbad/sim-id?Ident=4C+%2B37.11&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id">B2 0402+379</a> is a ‘fossil cluster,’ meaning it is the result of an entire <a href="https://en.wikipedia.org/wiki/Galaxy_cluster">galaxy cluster’s</a> worth of stars and gas merging into one single massive galaxy. Additionally, the presence of two supermassive black holes, coupled with their large combined mass, suggests they resulted from the amalgamation of multiple smaller black holes from multiple galaxies.</p>
<p>Following a galactic merger, supermassive black holes don’t collide head-on. Instead they begin slingshotting past each other as they settle into a bound orbit. With each pass they make, energy is transferred from the black holes to the surrounding stars. As they lose energy, the pair is dragged down closer and closer until they are just light-years apart, where gravitational radiation takes over and they merge. This process has been directly observed in pairs of <a href="https://en.wikipedia.org/wiki/Stellar_black_hole">stellar-mass black holes</a> — the <a href="https://en.wikipedia.org/wiki/First_observation_of_gravitational_waves">first ever recorded</a> instance being in 2015 via the detection of <a href="https://en.wikipedia.org/wiki/Gravitational_wave">gravitational waves</a> — but never in a binary of the supermassive variety.</p>
<p>With new knowledge of the system’s extremely large mass, the team concluded that an exceptionally large number of stars would have been needed to slow the binary’s orbit enough to bring them this close. In the process, the black holes seem to have flung out nearly all the matter in their vicinity, leaving the core of the galaxy starved of stars and gas. With no more material available to further slow the pair’s orbit, their merger has stalled in its final stages.</p>
<p><em>“Normally it seems that galaxies with lighter black hole pairs have enough stars and mass to drive the two together quickly,”</em> said Romani.<em> “Since this pair is so heavy it required lots of stars and gas to get the job done. But the binary has scoured the central galaxy of such matter, leaving it stalled and accessible for our study.”</em></p>
<p>Whether the pair will overcome their stagnation and eventually merge on timescales of millions of years, or continue in orbital limbo forever, is yet to be determined. If they do merge, the resulting gravitational waves would be a hundred million times more powerful than those produced by stellar-mass black hole mergers. It’s possible the pair could conquer that final distance via another galaxy merger, which would inject the system with additional material, or potentially a third black hole, to slow the pair’s orbit enough to merge. However, given B2 0402+379’s status as a fossil cluster, another galactic merger is unlikely.</p>
<p><em>“We’re looking forward to follow-up investigations of B2 0402+379’s core where we’ll look at how much gas is present,” </em>says Tirth Surti, Stanford undergraduate and the lead author on the paper.<em> “This should give us more insight into whether the supermassive black holes can eventually merge or if they will stay stranded as a binary.”</em></p>
<p><strong>Notes</strong></p>
<p>[1] While there is evidence of supermassive black holes coming within a few light-years of each other, it seems none have been able to overcome that final distance. The question of whether such an event is possible is known as the <a href="https://en.wikipedia.org/wiki/Binary_black_hole#Final-parsec_problem">final-parsec problem</a> and has been a topic of discussion amongst astronomers for decades. </p>
<p>[2] Previous observations have been made of galaxies containing two supermassive black holes, but in these cases they are thousands of light-years apart — too far to be in a bound orbit with one another like the binary found in B2 0402+379.</p>
<p>[3] Other black hole-powered sources exist with possible smaller separations, though these have been inferred using indirect observations and therefore can best be classified as candidate binaries.</p>
<p>[4] This theory was first put forth in 1980 by Begelman et al. and has long been argued to occur based on decades of observations of the centers of galaxies.</p>
<p><strong>More information</strong></p>
<p>This research was presented in a paper accepted in <em>The Astrophysical Journal</em>. DOI: 10.3847/1538-4357/ad14fa</p>
<p>The team is composed of: Tirth Surti (Kavli Institute for Particle Astrophysics and Cosmology, Stanford University), Roger W. Romani (Kavli Institute for Particle Astrophysics and Cosmology, Stanford University), Julia Scharwächter (Gemini Observatory/NSF’s NOIRLab), Alison Peck (University of Maryland) and Greg B. Taylor (University of New Mexico, Albuquerque).</p>
<p><a href="https://www.noirlab.edu/public/">NSF’s NOIRLab</a> (National Optical-Infrared Astronomy Research Laboratory), the US center for ground-based optical-infrared astronomy, operates the <a href="https://www.noirlab.edu/public/programs/gemini-observatory/">International Gemini Observatory</a> (a facility of <a href="https://www.nsf.gov/">NSF</a>, <a href="http://www.nrc-cnrc.gc.ca/eng/solutions/facilities/gemini.html">NRC–Canada</a>, <a href="http://www.conicyt.cl/astronomia/oficina-gemini-chile/">ANID–Chile</a>, <a href="https://www.gov.br/mcti/pt-br">MCTIC–Brazil</a>, <a href="http://www.geminiargentina.mincyt.gob.ar/">MINCyT–Argentina</a>, and <a href="http://kgmt.kasi.re.kr/kgmtscience">KASI–Republic of Korea</a>), Kitt Peak National Observatory (<a href="https://www.noirlab.edu/public/programs/kitt-peak-national-observatory/">KPNO</a>), Cerro Tololo Inter-American Observatory (<a href="https://www.noirlab.edu/public/programs/ctio/">CTIO</a>), the Community Science and Data Center (<a href="https://www.noirlab.edu/public/programs/csdc/">CSDC</a>), and <a href="https://www.noirlab.edu/public/programs/vera-c-rubin-observatory/">Vera C. Rubin Observatory</a> (operated in cooperation with the <a href="https://www.energy.gov/science/office-science">Department of Energy</a>’s <a href="https://www6.slac.stanford.edu/">SLAC</a> National Accelerator Laboratory). It is managed by the Association of Universities for Research in Astronomy (<a href="https://www.aura-astronomy.org/">AURA</a>) under a cooperative agreement with NSF and is headquartered in Tucson, Arizona. The astronomical community is honored to have the opportunity to conduct astronomical research on Iolkam Du’ag (Kitt Peak) in Arizona, on Maunakea in Hawai‘i, and on Cerro Tololo and Cerro Pachón in Chile. We recognize and acknowledge the very significant cultural role and reverence that these sites have to the Tohono O’odham Nation, to the Native Hawaiian community, and to the local communities in Chile, respectively.</p>
<p><strong>Links</strong></p>
<ul>
<li><a href="https://iopscience.iop.org/article/10.3847/1538-4357/ad14fa">Read the paper: The Central Kinematics and Black Hole Mass of 4C+37.11</a></li>
<li><a href="https://noirlab.edu/public/images/archive/category/gemini/?search=Gemini+North">Images of the Gemini North telescope</a></li>
<li><a href="https://noirlab.edu/public/videos/archive/search/?adv=&subject_name=Gemini%20North">Videos of the Gemini North telescope</a></li>
<li><a href="https://noirlab.edu/public/news/archive/search/?adv=&facility=1">Other Gemini North news</a></li>
<li><a href="https://noirlab.edu/public/news/archive/search/?instruments=31">Other discoveries made with GMOS-N</a></li>
<li><a href="https://noirlab.edu/public/news/archive/search/?release_type=1">Check out other NOIRLab Science Releases</a></li>
</ul>
<p><strong>Contacts</strong></p>
<p>Roger Romani<br />
Stanford University<br />
Email: <a href="mailto:rwr@astro.stanford.edu">rwr@astro.stanford.edu</a></p>
<p>Josie Fenske<br />
Jr. Public Information Officer<br />
NSF’s NOIRLab<br />
Email: <a href="mailto:josie.fenske@noirlab.edu">josie.fenske@noirlab.edu</a></p>
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<p>The merging of two supermassive black holes is a phenomenon that has long been predicted, though never directly observed. One theory put forth by astronomers is that these systems are so massive that they deplete their host galaxy of the stellar material needed to drive their merger. Using archival data from the Gemini North telescope, a team of astronomers have found a binary black hole that provides strong evidence supporting this idea. The team estimates the binary’s mass to be a whopping 28 billion times that of the Sun, qualifying the pair as the heaviest black hole binary ever measured. Not only does this measurement give valuable context to the formation of the binary system and the history of its host galaxy, but it supports the long-standing theory that the mass of a supermassive black hole binary plays a key role in stalling supermassive black hole mergers. <i>NOIRLab/NSF/AURA/J. daSilva/M. Zamani</i></p>
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Thu, 29 Feb 2024 19:35:21 +0000iromero22347 at https://www.gemini.eduhttps://www.gemini.edu/pr/astronomers-measure-heaviest-black-hole-pair-ever-found#commentsIGRINS-2 System Verification
https://www.gemini.edu/node/22342
<h2>IGRINS-2 System Verification</h2><h2 style="color:#DC143C;"><em><strong>News</strong></em></h2>
<p>February 2024: Call to join the Early Science Team (EST)</p>
<h3>Introduction</h3>
<p>The <a href="https://www.gemini.edu/instrumentation/future-instruments/igrins-2">IGRINS-2</a> System Verification observing run is planned for July 2024. The purpose of the run is to:</p>
<ul>
<li>perform end-to-end testing of the software, documentation, and operational procedures to prepare for instrument deployment (i.e. November IGRINS-2 Shared Risk Call for Fast Turnaround, Regular operations in 2025A and beyond); and</li>
<li>provide an initial set of publicly available observations to showcase the instrument capabilities, the range of science cases, and inform the community in preparation for the call for proposals.</li>
</ul>
<p>The International Gemini Observatory has allocated about 40 hours of engineering time for IGRINS-2 observations.</p>
<p>The Early Science Team (EST), which includes Gemini Observatory personnel and community representatives, will be responsible for developing the observations to take for the SV, reducing and analyzing the data, evaluating the observations, and presenting the results to support and promote the use of IGRINS-2 among the broader Gemini community. The EST is chosen in consultation with the Gemini Directorate, STAC, and the IGRINS-2 Instrument team.</p>
<p>Members of the Gemini community interested in joining the EST can self-nominate using this <a href="https://docs.google.com/forms/d/e/1FAIpQLSdx89NefECS8aY67eqTbWLL9VqPFpxBF1wqj4yOC1Rju-aRmQ/viewform">link</a>.</p>
<p>Regular updates on the IGRINS-2 System Verification observation planning and results will be presented on this page. An expected timeline is provided below.</p>
<p><strong>15 March 2024:</strong> Deadline for EST self-nomination.</p>
<p><strong>5 April 2024:</strong> EST composition is announced.</p>
<p><strong>May-June:</strong> SV Observing plan (with priority) is finalized (the EST tests the Integration Time Calculator and the Phase I Tool software; the SV team tests the Observing Tool). The Target list is released to the community.</p>
<p><strong>July:</strong> Observations will be performed around 17–23 July. Description of the observations is released.</p>
<p><strong>August:</strong> Raw data released. Data quality evaluation released.</p>
<p><strong>September-October:</strong> Reduced data released. </p>
<p><strong>November:</strong> IGRINS-2 will be offered in Shared Risk for Fast Turnaround proposals.</p>
<h3>IGRINS-2 Modes to be showcased in the SV run</h3>
<p>Young Stellar Objects and their disks<br />
Young planets and Brown Dwarfs<br />
Binary Systems<br />
Galactic Evolution<br />
Interstellar medium<br />
AGNs<br />
Other</p>
<h3>Acknowledgment to include in papers using IGRINS-2 SV data</h3>
<p>Please include the following acknowledgment in any paper that makes use of IGRINS-2 SV data, in addition to the general Gemini acknowledgment (see <a href="https://noirlab.edu/science/about/scientific-acknowledgments">Section 8.2 here</a>).</p>
<p><em>“This work used the Immersion Grating Infrared Spectrograph 2 (IGRINS-2) developed and built by a collaboration between Korea Astronomy and Space Science Institute (KASI) and the International Gemini Observatory.” </em></p>
<div class="label-above">Instrument</div>IGRINS-2Tue, 13 Feb 2024 19:03:59 +0000iromero22342 at https://www.gemini.eduhttps://www.gemini.edu/node/22342#commentsIGRINS-2 System Verification
https://www.gemini.edu/instrumentation/future-instruments/igrins-2/igrins-2-system-verification
<h2>IGRINS-2 System Verification</h2><h2 style="color:#DC143C;"><em><strong>News</strong></em></h2>
<p>February 2024: Call to join the Early Science Team (EST)</p>
<hr />
<h2>Introduction</h2>
<hr />
<p>The <a href="https://www.gemini.edu/instrumentation/future-instruments/igrins-2">IGRINS-2</a> System Verification observing run is planned for July 2024. The purpose of the run is to:</p>
<ul>
<li>perform end-to-end testing of the software, documentation, and operational procedures to prepare for instrument deployment (i.e. November IGRINS-2 Shared Risk Call for Fast Turnaround, Regular operations in 2025A and beyond); and</li>
<li>provide an initial set of publicly available observations to showcase the instrument capabilities, the range of science cases, and inform the community in preparation for the call for proposals.</li>
</ul>
<p>The International Gemini Observatory has allocated about 40 hours of engineering time for IGRINS-2 observations.</p>
<p>The Early Science Team (EST), which includes Gemini Observatory personnel and community representatives, will be responsible for developing the observations to take for the SV, reducing and analyzing the data, evaluating the observations, and presenting the results to support and promote the use of IGRINS-2 among the broader Gemini community. The EST is chosen in consultation with the Gemini Directorate, STAC, and the IGRINS-2 Instrument team.</p>
<p>Members of the Gemini community interested in joining the EST can self-nominate using this <a href="https://docs.google.com/forms/d/e/1FAIpQLSdx89NefECS8aY67eqTbWLL9VqPFpxBF1wqj4yOC1Rju-aRmQ/viewform">link</a>.</p>
<p>Regular updates on the IGRINS-2 System Verification observation planning and results will be presented on this page. An expected timeline is provided below.</p>
<p><strong>15 March 2024:</strong> Deadline for EST self-nomination.</p>
<p><strong>5 April 2024:</strong> EST composition is announced.</p>
<p><strong>May-June:</strong> SV Observing plan (with priority) is finalized (the EST tests the Integration Time Calculator and the Phase I Tool software; the SV team tests the Observing Tool). The Target list is released to the community.</p>
<p><strong>July:</strong> Observations will be performed around 17–23 July. Description of the observations is released.</p>
<p><strong>August:</strong> Raw data released. Data quality evaluation released.</p>
<p><strong>September-October:</strong> Reduced data released. </p>
<p><strong>November:</strong> IGRINS-2 will be offered in Shared Risk for Fast Turnaround proposals.</p>
<hr />
<h2>IGRINS-2 science cases</h2>
<hr />
<p>Young Stellar Objects and their disks<br />
Young planets and Brown Dwarfs<br />
Binary Systems<br />
Galactic Evolution<br />
Interstellar medium<br />
AGNs</p>
<hr />
<h2>Acknowledgment to include in papers using IGRINS-2 SV data</h2>
<hr />
<p>Please include the following acknowledgment in any paper that makes use of IGRINS-2 SV data, in addition to the general Gemini acknowledgment (see <a href="https://noirlab.edu/science/about/scientific-acknowledgments">Section 8.2 here</a>).</p>
<p><em>“This work used the Immersion Grating Infrared Spectrograph 2 (IGRINS-2) developed and built by a collaboration between Korea Astronomy and Space Science Institute (KASI) and the International Gemini Observatory.” </em></p>
<div class="label-above">Instrument</div>IGRINS-2Tue, 13 Feb 2024 18:59:27 +0000iromero22341 at https://www.gemini.eduhttps://www.gemini.edu/instrumentation/future-instruments/igrins-2/igrins-2-system-verification#commentsStatus Notes
https://www.gemini.edu/news/general-announcements/status-notes
<p>While Gemini is once again observing after the <a href="https://www.gemini.edu/news/general-announcements/cybersecurity-incident-nsf-s-noirlab">Cyber Incident</a>, there are some operational issues which we are still working out. We are writing to inform you of the operational limitations we are working under while work continues.</p>
<p>In particular, some of the usual tools for communicating program status are currently unavailable or not fully functional, and we are actively working to minimize the impact on users.</p>
<p>Due to the Cyber Incident, it is possible that emails or other communications (from the <a href="https://www.gemini.edu/observing/phase-ii/ot">Observing Tool</a>) may have been lost. If you, as a Principal Investigator, have not received an expected response, please get in touch with your Contact Scientist directly. Feel free to make as much contact as you need, and kind reminders to your <a href="https://www.gemini.edu/about/contact-us/gemini-contact-scientists">Contact Scientists</a> are always welcome.</p>
<p>We are aware that some programs with early targets were impacted by the initial shutdown period. <a href="https://www.gemini.edu/observing/phase-i/standard-semester-program#Persistent">Band 1 programs will persist for one semester as usual</a>, and we will make a best effort for programs associated with Ph.D. Theses. Fast Turnaround (<a href="https://www.gemini.edu/observing/phase-i/ft">FT</a>) and Director's Discretionary (<a href="https://www.gemini.edu/observing/phase-i/ddt">DD</a>) time may provide alternative routes for completing programs.</p>
<p>We appreciate your understanding and cooperation during what continues to be a challenging time. If you have any further questions or concerns, do not hesitate to reach out to your Contact Scientist.</p>
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</section>Tue, 16 Jan 2024 07:09:21 +0000astephens22335 at https://www.gemini.eduhttps://www.gemini.edu/news/general-announcements/status-notes#commentsError | Gemini Observatory