pith. sign in

arxiv: 2606.05811 · v1 · pith:QH4ACHTEnew · submitted 2026-06-04 · 🌌 astro-ph.IM · astro-ph.SR

Observing the integrated and spatially resolved Sun with ultra-high spectral resolution

S. Sch\"afer , K. Royen , A. Huster Zapke , M. Ellwarth , A. Reiners This is my paper

Pith reviewed 2026-06-27 23:47 UTC · model grok-4.3

classification 🌌 astro-ph.IM astro-ph.SR
keywords solar spectroscopylaser frequency combFourier transform spectrographconvective blueshiftSun-as-a-starhigh resolution spectroscopyfrequency calibration
0
0 comments X

The pith

A solar instrument suite provides frequency calibration accurate to less than 10 cm/s across 400-800 nm for precision spectroscopy.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper describes a solar observatory that combines a 50 cm siderostat with a vacuum vertical telescope, a Fourier transform spectrograph with resolution exceeding 900,000 at 600 nm, and a laser frequency comb for calibration. The setup can observe either the integrated Sun or a 32.5 arcsecond field of view on the solar surface by guiding light into a fiber. The key feature is the frequency calibration that remains accurate to better than 10 cm/s over the 400-800 nm range. This capability allows detailed investigation of spectral line variability in Sun-as-a-star observations and the convective blueshift on the solar surface using many lines.

Core claim

Our instrument suite can deliver spectroscopic measurements with extremely accurate frequency calibration, which is valid across very large frequency regions (approx. 400-800 nm in wavelength). This allows precision spectroscopy of individual lines in order to study the variability of spectral lines in Sun-as-a-star observations as well as determining the convective blueshift across the solar surface from many spectral lines.

What carries the argument

The laser frequency comb that achieves frequency calibration accurate to less than 10 cm/s, paired with the high-resolution Fourier transform spectrograph.

If this is right

  • The calibration supports Sun-as-a-star observations to track spectral line variability.
  • Many spectral lines can be used to map convective blueshift across the solar surface.
  • The wide wavelength coverage enables analysis without separate calibrations for different bands.
  • Spatially resolved observations are possible by injecting light from specific solar positions.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Similar calibration techniques could be applied to other solar observatories to improve consistency in measurements.
  • The precision might allow detection of subtle changes in solar activity through line profile analysis.
  • If the system proves stable, it could serve as a reference for validating models of solar convection.

Load-bearing premise

The laser frequency comb maintains its accuracy of less than 10 cm/s across the full 400-800 nm range during actual observations.

What would settle it

Observing a known spectral line with established wavelength and checking if the measured position matches within the claimed precision would test the calibration.

Figures

Figures reproduced from arXiv: 2606.05811 by A. Huster Zapke, A. Reiners, K. Royen, M. Ellwarth, S. Sch\"afer.

Figure 1
Figure 1. Figure 1: Rooftop: 50 cm siderostat with vertical vacuum telescope, integrated Sun setup with integrating sphere, 50 cm [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Siderostat on the roof, view southbound towards the city center of G [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Zemax simulation of the resolved Sun setup, starting at the Nasmyth focus (1) and ending at the camera position [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: The solar disc as seen by the detector (including flat-field correction). Both, the hole from the Nasmyth mirror [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Segment of the solar spectrum plotted in vacuum wavelength. Spectra for three di [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Radial velocities of eight solar surface regions [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 8
Figure 8. Figure 8: Schematic view of the different coordinate systems used during frame transformations. Orange: Sun’s (lon, lat)-coordinates. Blue (curved): absolute topocentric coordinates. Green: Projected Plane coordinates. Red: Native coordinates. 6.2 Frame transformation: Sun to Image Computing the camera pixel coordinates of a sun-feature is the result of a mapping chain that transforms some solar-surface input coordi… view at source ↗
Figure 9
Figure 9. Figure 9: Astrometric coordinate transformation steps from solar Helioprojective radial to Refracted topocentric coordinates. [PITH_FULL_IMAGE:figures/full_fig_p010_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Instrumental coordinate transformation steps from real world coordinates to pixel coordinates in the camera [PITH_FULL_IMAGE:figures/full_fig_p010_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Overview of the siderostat-specific coordinate transformations for a spatially extended target (Sun or Moon). See [PITH_FULL_IMAGE:figures/full_fig_p011_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: For several positions at the sky, represented by the points in the left image, measurements of the roll angle [PITH_FULL_IMAGE:figures/full_fig_p012_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Comparison between measured pointing errors from moon observations (blue points) and analytical uncertainty [PITH_FULL_IMAGE:figures/full_fig_p014_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Movable arm containing the integrated Sun setup: The flat mirror (1) is placed in the center of the beam coming [PITH_FULL_IMAGE:figures/full_fig_p017_14.png] view at source ↗
read the original abstract

The Institute for Astrophysics G\"ottingen operates a solar observatory that combines a 50\,cm siderostat with (1) a vacuum vertical telescope, (2) a very high resolution Fourier Transform Spectrograph ($R > 900,000$ at 600\,nm), and (3) a Laser Frequency Comb for extremely precise and accurate frequency calibration ($<10\,cm/s$). We introduce our setup that feeds the spectrograph with either a 32.5" field of view of the solar surface, or with disk-integrated sunlight for Sun-as-a-star observations and explain the necessary computational steps to guide specific positions on the solar surface into the fiber. Our instrument suite can deliver spectroscopic measurements with extremely accurate frequency calibration, which is valid across very large frequency regions (approx. 400-800\,nm in wavelength). This allows precision spectroscopy of individual lines in order to study the variability of spectral lines in Sun-as-a-star observations as well as determining the convective blueshift across the solar surface from many spectral lines.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 1 minor

Summary. The paper describes a solar observatory at the Institute for Astrophysics Göttingen that combines a 50 cm siderostat, vacuum vertical telescope, Fourier Transform Spectrograph (R > 900,000 at 600 nm), and Laser Frequency Comb (<10 cm/s calibration). It explains the optical feed for either a 32.5 arcsecond solar surface field or disk-integrated sunlight, plus computational guiding steps, and asserts that the suite enables precision spectroscopy of individual lines across ~400-800 nm for Sun-as-a-star line variability studies and spatially resolved convective blueshift measurements.

Significance. If the stated calibration performance is realized under operational conditions, the instrument would offer a distinctive capability for high-precision solar spectroscopy, supporting studies of spectral line variability and surface convection that are relevant to stellar activity and radial-velocity exoplanet work.

major comments (1)
  1. [Abstract] Abstract and main text: the assertion that the LFC delivers <10 cm/s accuracy valid across the full 400-800 nm range is presented without an error budget, on-sky validation data, or tests of fiber-injection stability, guiding residuals, or modal noise under the siderostat + vacuum-telescope feed; this accuracy is load-bearing for the two science applications claimed.
minor comments (1)
  1. The description of the fiber-injection and guiding system would benefit from additional quantitative detail on throughput, position repeatability, and how the 32.5 arcsecond field is maintained.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their detailed review and constructive feedback. The major comment raises a valid point about the presentation of the LFC calibration accuracy. We address it below and will revise the manuscript accordingly to strengthen the supporting details for the claimed performance.

read point-by-point responses

  1. Referee: [Abstract] Abstract and main text: the assertion that the LFC delivers <10 cm/s accuracy valid across the full 400-800 nm range is presented without an error budget, on-sky validation data, or tests of fiber-injection stability, guiding residuals, or modal noise under the siderostat + vacuum-telescope feed; this accuracy is load-bearing for the two science applications claimed.

    Authors: We agree that the manuscript currently states the <10 cm/s figure without a full error budget or on-sky validation data. This value originates from the LFC design specifications and our laboratory characterizations demonstrating stability across 400-800 nm. However, the referee is correct that integration-specific factors such as fiber-injection stability, guiding residuals, and modal noise under the actual optical feed are not quantified in the present version. In revision we will add a dedicated subsection providing the available error budget from lab measurements, with explicit discussion of the known contributions and limitations. We will also clarify that comprehensive on-sky validation remains part of commissioning and is reserved for a follow-up paper. This revision directly supports the two science applications by making the basis of the accuracy claim transparent while preserving the instrument-description focus of the current work. revision: yes

Circularity Check

0 steps flagged

No significant circularity; instrument description only

full rationale

The paper is an instrument description that states performance specifications (LFC <10 cm/s calibration across 400-800 nm) and outlines setup/computational guidance steps without presenting any derivation chain, equations, or fitted quantities. No load-bearing claims reduce to self-definition, fitted inputs renamed as predictions, or self-citation chains. The central accuracy claim is presented as a design specification rather than a derived result, so no circularity patterns apply.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

No free parameters, axioms, or invented entities; the paper is a description of an observational facility rather than a theoretical derivation.

pith-pipeline@v0.9.1-grok · 5727 in / 1091 out tokens · 19026 ms · 2026-06-27T23:47:53.651853+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

54 extracted references · 40 canonical work pages · 5 internal anchors

  1. [1]

    , keywords =

    Radial velocity observations of the sun at night. , keywords =. doi:10.1086/172251 , adsurl =

    work page doi:10.1086/172251

  2. [2]

    , archivePrefix = "arXiv", eprint =

    Correlations between sunspots and their moat flows. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201220543 , adsurl =

    work page doi:10.1051/0004-6361/201220543

  3. [3]

    , archivePrefix = "arXiv", eprint =

    A Magnetic Calibration of Photospheric Doppler Velocities. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/765/2/98 , adsurl =

    work page doi:10.1088/0004-637x/765/2/98

  4. [4]

    , keywords =

    Wavelength Dependence of the Helioseismic and Magnetic Imager (HMI) Instrument onboard the Solar Dynamics Observatory (SDO). , keywords =. doi:10.1007/s11207-011-9723-8 , adsurl =

    work page doi:10.1007/s11207-011-9723-8

  5. [5]

    , archivePrefix = "arXiv", eprint =

    The Sun as a planet-host star: proxies from SDO images for HARPS radial-velocity variations. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stw187 , adsurl =

    work page doi:10.1093/mnras/stw187

  6. [6]

    , archivePrefix = "arXiv", eprint =

    Toward Understanding Stellar Radial Velocity Jitter as a Function of Wavelength: The Sun as a Proxy. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/798/1/63 , adsurl =

    work page doi:10.1088/0004-637x/798/1/63

  7. [7]

    , archivePrefix = "arXiv", eprint =

    SOAP 2.0: A Tool to Estimate the Photometric and Radial Velocity Variations Induced by Stellar Spots and Plages. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/796/2/132 , adsurl =

    work page doi:10.1088/0004-637x/796/2/132

  8. [8]

    , archivePrefix = "arXiv", eprint =

    Photospheric activity, rotation, and radial velocity variations of the planet-hosting star CoRoT-7. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201014403 , adsurl =

    work page doi:10.1051/0004-6361/201014403

  9. [9]

    , archivePrefix = "arXiv", eprint =

    Reconstructing the solar integrated radial velocity using MDI/SOHO. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201014199 , adsurl =

    work page doi:10.1051/0004-6361/201014199

  10. [10]

    Using the Sun to estimate Earth-like planets detection capabilities . II. Impact of plages. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/200913551 , adsurl =

    work page doi:10.1051/0004-6361/200913551

  11. [11]

    Using the Sun to estimate Earth-like planets detection capabilities . I. Impact of cold spots. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/200913071 , adsurl =

    work page doi:10.1051/0004-6361/200913071

  12. [12]

    , keywords =

    Magnetic fields, convection and solar luminosity variability. , keywords =. doi:10.1038/297208a0 , adsurl =

    work page doi:10.1038/297208a0

  13. [13]

    , keywords =

    Solar granulation - Influence of convection on spectral line asymmetries and wavelength shifts. , keywords =

  14. [14]

    II - The effect of granular motions

    Some comments on the limb shift of solar lines. II - The effect of granular motions. , keywords =. doi:10.1007/BF00157270 , adsurl =

    work page doi:10.1007/bf00157270

  15. [15]

    o ttingen Solar Radial Velocity Project: Sub-m s ^ -1 Doppler Precision from FTS Observations of the Sun as a Star. , archivePrefix =

    The G \"o ttingen Solar Radial Velocity Project: Sub-m s ^ -1 Doppler Precision from FTS Observations of the Sun as a Star. , archivePrefix = "arXiv", eprint =. doi:10.1088/1538-3873/128/967/095002 , adsurl =

    work page doi:10.1088/1538-3873/128/967/095002

  16. [16]

    , archivePrefix = "arXiv", eprint =

    HARPS-N Observes the Sun as a Star. , archivePrefix = "arXiv", eprint =. doi:10.1088/2041-8205/814/2/L21 , adsurl =

    work page doi:10.1088/2041-8205/814/2/l21 2041

  17. [17]

    I - 1983-1985

    On the apparent velocity of integrated sunlight. I - 1983-1985. , keywords =. doi:10.1086/165242 , adsurl =

    work page doi:10.1086/165242 1983

  18. [18]

    2: 1983-1992 and comparisons with magnetograms

    On the apparent velocity of integrated sunlight. 2: 1983-1992 and comparisons with magnetograms. , keywords =. doi:10.1086/174074 , adsurl =

    work page doi:10.1086/174074 1983

  19. [19]

    Advances in Space Research , keywords =

    The radial velocity of the sun as a star and the solar cycle. Advances in Space Research , keywords =. doi:10.1016/0273-1177(86)90415-1 , adsurl =

    work page doi:10.1016/0273-1177(86)90415-1

  20. [20]

    Three years of Sun-as-a-star radial-velocity observations on the approach to solar minimum

    Three years of Sun-as-a-star radial-velocity observations on the approach to solar minimum. , keywords =. doi:10.1093/mnras/stz1215 , archivePrefix =. 1904.12186 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz1215 1904

  21. [21]

    arXiv e-prints , keywords =

    Three Years of HARPS-N High-Resolution Spectroscopy and Precise Radial Velocity Data for the Sun. arXiv e-prints , keywords =

  22. [22]

    and Mrotzek, N

    Reiners, A. and Mrotzek, N. and Lemke, U. and Hinrichs, J. and Reinsch, K. , year=. The IAG solar flux atlas: Accurate wavelengths and absolute convective blueshift in standard solar spectra , volume=. doi:10.1051/0004-6361/201527530 , journal=

    work page doi:10.1051/0004-6361/201527530

  23. [23]

    Solar flux atlas from 296 to 1300 nm

  24. [24]

    , keywords =

    An Optical and Near-infrared (2958-9250 A ) Solar Flux Atlas. , keywords =. doi:10.1088/0067-0049/195/1/6 , adsurl =

    work page doi:10.1088/0067-0049/195/1/6

  25. [25]

    10.1051/0004-6361/201322324

    A frequency comb calibrated solar atlas , DOI= "10.1051/0004-6361/201322324", url= "https://doi.org/10.1051/0004-6361/201322324", journal =

    work page doi:10.1051/0004-6361/201322324

  26. [26]

    , keywords =

    Coordinate systems for solar image data. , keywords =. doi:10.1051/0004-6361:20054262 , adsurl =

    work page doi:10.1051/0004-6361:20054262

  27. [27]

    Celestial Mechanics and Dynamical Astronomy , keywords =

    Report of the IAU/IAG Working Group on cartographic coordinates and rotational elements: 2006. Celestial Mechanics and Dynamical Astronomy , keywords =. doi:10.1007/s10569-007-9072-y , adsurl =

    work page doi:10.1007/s10569-007-9072-y 2006

  28. [28]

    , keywords =

    The International Celestial Reference Frame as Realized by Very Long Baseline Interferometry. , keywords =. doi:10.1086/300408 , adsurl =

    work page doi:10.1086/300408

  29. [29]

    A Giant Step: from Milli- to Micro-arcsecond Astrometry , year = 2008, editor =

    Definition and realization of the celestial intermediate reference system. A Giant Step: from Milli- to Micro-arcsecond Astrometry , year = 2008, editor =. doi:10.1017/S1743921308019583 , adsurl =

    work page doi:10.1017/s1743921308019583 2008

  30. [30]

    Representations of celestial coordinates in FITS

    Representations of celestial coordinates in FITS. , keywords =. doi:10.1051/0004-6361:20021327 , archivePrefix =. astro-ph/0207413 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20021327

  31. [31]

    Huke and M

    P. Huke and M. Debus and M. Zechmeister and A. Reiners , journal =. Characterization and calibration of a Fourier-transform spectrometer using a laser frequency comb , volume =. 2019 , url =. doi:10.1364/JOSAB.36.001899 , abstract =

    work page doi:10.1364/josab.36.001899 2019

  32. [32]

    Phase-correction algorithm for Fourier transform spectroscopy of a laser frequency comb , volume =

    Philipp Huke and Michael Debus and Ansgar Reiners , journal =. Phase-correction algorithm for Fourier transform spectroscopy of a laser frequency comb , volume =. 2019 , url =. doi:10.1364/JOSAB.36.001260 , abstract =

    work page doi:10.1364/josab.36.001260 2019

  33. [33]

    Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation III , editor =

    Michael Debus and Philipp Huke and Grzegorz Kowzan and Piotr Masłowski and Ansgar Reiners , title =. Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation III , editor =. 2018 , doi =

    2018

  34. [34]

    10.1051/0004-6361/201629088

    Radial velocity observations of the 2015 Mar. 20 eclipse - A benchmark Rossiter-McLaughlin curve with zero free parameters , DOI= "10.1051/0004-6361/201629088", url= "https://doi.org/10.1051/0004-6361/201629088", journal =

    work page doi:10.1051/0004-6361/201629088 2015

  35. [35]

    Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation II , editor =

    Philipp Huke and Lev Tal-Or and Luis Fernando Sarmiento and Ansgar Reiners , title =. Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation II , editor =. 2016 , doi =

    2016

  36. [36]

    I: instrument and survey overview

    CARMENES. I: instrument and survey overview. Ground-based and Airborne Instrumentation for Astronomy IV , year = 2012, editor =. doi:10.1117/12.925164 , adsurl =

    work page doi:10.1117/12.925164 2012

  37. [37]

    The Messenger , year = 2003, month = dec, volume =

    Setting New Standards with HARPS. The Messenger , year = 2003, month = dec, volume =

    2003

  38. [38]

    Numerically stable direct least squares fitting of ellipses , author=. Proc. 6th International Conference in Central Europe on Computer Graphics and Visualization. WSCG , volume=. 1998 , organization=

    1998

  39. [39]

    IEEE Transactions on Pattern Analysis and Machine Intelligence , title=

    J. IEEE Transactions on Pattern Analysis and Machine Intelligence , title=. 1986 , volume=

    1986

  40. [40]

    and Millman, K

    Charles R. Harris and K. Jarrod Millman and St. Array programming with. 2020 , month = sep, journal =. doi:10.1038/s41586-020-2649-2 , publisher =

    work page doi:10.1038/s41586-020-2649-2 2020

  41. [41]

    , citeulike-article-id =

    Bradski, G. , citeulike-article-id =. Dr. Dobb's Journal of Software Tools , keywords =

  42. [42]

    2010 , volume=

    2010 International Conference on Computer Application and System Modeling (ICCASM 2010) , title=. 2010 , volume=

    2010

  43. [43]

    Convective blueshifts in the solar atmosphere. III. High-accuracy observations of spectral lines in the visible. , keywords =. doi:10.1051/0004-6361/201834925 , archivePrefix =. 1901.07606 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201834925 1901

  44. [44]

    Precision spectroscopy with a frequency-comb-calibrated solar spectrograph

  45. [45]

    , year = 1996, month = jan, volume =

    Ancillary data services of NASA's Navigation and Ancillary Information Facility. , year = 1996, month = jan, volume =. doi:10.1016/0032-0633(95)00107-7 , adsurl =

    work page doi:10.1016/0032-0633(95)00107-7 1996

  46. [46]

    , keywords =

    Rotation of Doppler Features in the Solar Photosphere. , keywords =. doi:10.1086/168467 , adsurl =

    work page doi:10.1086/168467

  47. [47]

    Fiber-coupling of Fourier Transform Spectrographs , booktitle =

  48. [48]

    IAU SOFA Software Collection

    SOFA. IAU SOFA Software Collection

  49. [49]

    The Astrophysical Journal , volume=

    The sunpy project: Open source development and status of the version 1.0 core package , author=. The Astrophysical Journal , volume=. 2020 , publisher=

    2020

  50. [50]

    Astropy: A Community Python Package for Astronomy

    doi:10.1051/0004-6361/201322068 , Eid =. arXiv , Author =:1307.6212 , Journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322068

  51. [51]

    The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

    The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. aj , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aabc4f

  52. [52]

    Mumford and Nabil Freij and Steven Christe and Jack Ireland and Florian Mayer and V

    Stuart J. Mumford and Nabil Freij and Steven Christe and Jack Ireland and Florian Mayer and V. Keith Hughitt and Albert Y. Shih and Daniel F. Ryan and Simon Liedtke and David Stansby and David Pérez-Suárez and Vishnunarayan K I. and Pritish Chakraborty and Andrew Inglis and Punyaslok Pattnaik and Brigitta Sipőcz and Laura Hayes and Rishabh Sharma and Andr...

    work page doi:10.5281/zenodo.3940415

  53. [53]

    Smith and Maria T

    David E. Smith and Maria T. Zuber and Gregory A. Neumann and Erwan Mazarico and Frank G. Lemoine and James W. Head III and Paul G. Lucey and Oded Aharonson and Mark S. Robinson and Xiaoli Sun and Mark H. Torrence and Michael K. Barker and Juergen Oberst and Thomas C. Duxbury and Dandan Mao and Olivier S. Barnouin and Kopal Jha and David D. Rowlands and Sa...

    work page doi:10.1016/j.icarus.2016.06.006 2017

  54. [54]

    and Robinson, M

    Sato, H. and Robinson, M. S. and Hapke, B. and Denevi, B. W. and Boyd, A. K. , title =. Journal of Geophysical Research: Planets , volume =. doi:https://doi.org/10.1002/2013JE004580 , url =. https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1002/2013JE004580 , abstract =

    work page doi:10.1002/2013je004580