For Publishers
DiscoveryMetadataPeer reviewHostingPublishing
For Researchers
JoinPublishReviewCollect
Register
Blog
About
Search
Advanced search
My ScienceOpen
Search
For Publishers
For Researchers
Blog
About
10
views
3
references
 Top references
cited by
1
    
0 reviews
 Review
0
comments
 Comment
0
recommends
+1 Recommend
0 collections
    0
    shares
      149
      similar
       All similar
      • Record: found
      • Abstract: found
      • Article: found
      Is Open Access

      Development and construction of MAROON-X

      Preprint

      Read this article at

      ScienceOpenArXiv
      Bookmark
          There is no author summary for this article yet. Authors can add summaries to their articles on ScienceOpen to make them more accessible to a non-specialist audience.

          Abstract

          We report on the development and construction of a new fiber-fed, red-optical, high-precision radial-velocity spectrograph for one of the twin 6.5m Magellan Telescopes in Chile. MAROON-X will be optimized to find and characterize rocky planets around nearby M dwarfs with an intrinsic per measurement noise floor below 1 m/s. The instrument is based on a commercial echelle spectrograph customized for high stability and throughput. A microlens array based pupil slicer and double scrambler, as well as a rubidium-referenced etalon comb calibrator will turn this spectrograph into a high-precision radial-velocity machine. MAROON-X will undergo extensive lab tests in the second half of 2016.

          Related collections

          Most cited references3

          • Record: found
          • Abstract: found
          • Article: found
          Is Open Access

          Detecting Planets Around Very Low Mass Stars with the Radial Velocity Method

          A. Reiners, A. Seifahrt, K. Huber … (2009)
          The detection of planets around very low-mass stars with the radial velocity method is hampered by the fact that these stars are very faint at optical wavelengths where the most high-precision spectrometers operate. We investigate the precision that can be achieved in radial velocity measurements of low mass stars in the near infrared (nIR) Y-, J-, and H-bands, and we compare it to the precision achievable in the optical. For early-M stars, radial velocity measurements in the nIR offer no or only marginal advantage in comparison to optical measurements. Although they emit more flux in the nIR, the richness of spectral features in the optical outweighs the flux difference. We find that nIR measurement can be as precise than optical measurements in stars of spectral type ~M4, and from there the nIR gains in precision towards cooler objects. We studied potential calibration strategies in the nIR finding that a stable spectrograph with a ThAr calibration can offer enough wavelength stability for m/s precision. Furthermore, we simulate the wavelength-dependent influence of activity (cool spots) on radial velocity measurements from optical to nIR wavelengths. Our spot simulations reveal that the radial velocity jitter does not decrease as dramatically towards longer wavelengths as often thought. The jitter strongly depends on the details of the spots, i.e., on spot temperature and the spectral appearance of the spot. Forthcoming nIR spectrographs will allow the search for planets with a particular advantage in mid- and late-M stars. Activity will remain an issue, but simultaneous observations at optical and nIR wavelengths can provide strong constraints on spot properties in active stars.
          Article 0 comments Cited 14 times – based on 0 reviews
          Preprint
               Review now
            Bookmark
            • Record: found
            • Abstract: found
            • Article: found
            Is Open Access

            Maximizing the ExoEarth Candidate Yield from a Future Direct Imaging Mission

            , , … (2014)
            ExoEarth yield is a critical science metric for future exoplanet imaging missions. Here we estimate exoEarth candidate yield using single visit completeness for a variety of mission design and astrophysical parameters. We review the methods used in previous yield calculations and show that the method choice can significantly impact yield estimates as well as how the yield responds to mission parameters. We introduce a method, called Altruistic Yield Optimization, that optimizes the target list and exposure times to maximize mission yield, adapts maximally to changes in mission parameters, and increases exoEarth candidate yield by up to 100% compared to previous methods. We use Altruistic Yield Optimization to estimate exoEarth candidate yield for a large suite of mission and astrophysical parameters using single visit completeness. We find that exoEarth candidate yield is most sensitive to telescope diameter, followed by coronagraph inner working angle, followed by coronagraph contrast, and finally coronagraph contrast noise floor. We find a surprisingly weak dependence of exoEarth candidate yield on exozodi level. Additionally, we provide a quantitative approach to defining a yield goal for future exoEarth-imaging missions.
            Article 0 comments Cited 6 times – based on 0 reviews
            Preprint
                 Review now
              Bookmark
              • Record: found
              • Abstract: found
              • Article: found
              Is Open Access

              Science Parametrics for Missions to Search for Earthlike Exoplanets by Direct Imaging

              Robert A Brown (2014)
              We use \(N_{t}\), the number of exoplanets observed in time \(t\), as a science metric to study direct-search missions like Terrestrial Planet Finder. In our model, \(N\) has 27 parameters, divided into three categories: 2 astronomical, 7 instrumental, and 18 science-operational. For various "27-vectors" of those parameters chosen to explore parameter space, we compute design reference missions to estimate \(N_{t}\). Our treatment includes the recovery of completeness \(c\) after a search observation, for revisits, solar and antisolar avoidance, observational overhead, and follow-on spectroscopy. Our baseline 27-vector has aperture \(D = 16\)m, inner working angle \(IWA = 0.039''\), mission time \(t = 0-5\) years, occurrence probability for earthlike exoplanets \(\eta = 0.2\), and typical values for the remaining 23 parameters. For the baseline case, a typical five-year design reference mission has an input catalog of \(\sim\)4700 stars with nonzero completeness, \(\sim\)1300 unique stars observed in \(\sim\)2600 observations, of which \(\sim\)1300 are revisits, and it produces \(N_{1}\sim50\) exoplanets after one year and \(N_{5}\sim130\) after five years. We explore offsets from the baseline for ten parameters. We find that \(N\) depends strongly on \(IWA\) and only weakly on \(D\). It also depends only weakly on zodiacal light for \(Z 0.2\), and scattered starlight for \(\zeta < 10^{-10}\). We find that observational overheads, completeness recovery and revisits, solar and antisolar avoidance, and follow-on spectroscopy are all important factors in estimating \(N\).
              Article 0 comments Cited 1 times – based on 0 reviews
              Preprint
                   Review now
                Bookmark
                All references

                Author and article information

                Journal
                Publication date Created: 2016-06-22
                Article
                ArXiV ID: 1606.07140
                SO-VID: 8e3e6362-39a9-4c4e-b1c0-280acae25ea6
                License:

                http://arxiv.org/licenses/nonexclusive-distrib/1.0/

                History
                Custom metadata
                Comments 14 pages, 10 figures, submitted to SPIE Astronomical Telescopes & Instrumentation 2016 (9908-45)
                Categories astro-ph.IM astro-ph.EP

                ScienceOpen disciplines: Planetary astrophysics,Instrumentation & Methods for astrophysics
                Data availability:
                ScienceOpen disciplines: Planetary astrophysics, Instrumentation & Methods for astrophysics

                Comments

                Comment on this article