ESPRESSO

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ESPRESSO spectrograph concept at the Preliminary Design Review. ESPRESSO spectrograph concept at the Preliminary Design Review..jpg
ESPRESSO spectrograph concept at the Preliminary Design Review.
ESPRESSO spectrograph optical design at the Preliminary Design Review. ESPRESSO spectrograph optical design at the Preliminary Design Review..jpg
ESPRESSO spectrograph optical design at the Preliminary Design Review.
ESPRESSO successfully made its first observations in November 2017.

ESPRESSO (Echelle Spectrograph for Rocky Exoplanet- and Stable Spectroscopic Observations) [1] is a third-generation, fiber fed, cross-dispersed, echelle spectrograph mounted on the European Southern Observatory's Very Large Telescope (VLT). The unit saw its first light with one VLT in December 2017 and first light with all four VLT units in February 2018. [2]

Contents

ESPRESSO is the successor of a line of echelle spectrometers that include CORAVEL, Elodie, Coralie, and HARPS. It measures changes in the light spectrum with great sensitivity, and is being used to search for Earth-size rocky exoplanets via the radial velocity method. For example, Earth induces a radial-velocity variation of 9 cm/s on the Sun; this gravitational "wobble" causes minute variations in the color of sunlight, invisible to the human eye but detectable by the instrument. [3] The telescope light is fed to the instrument, located in the VLT Combined-Coude Laboratory 70 meters away from the telescope, where the light from up to four unit telescopes of the VLT can be combined.

Sensitivity

Data from ESPRESSO First Light. ESPRESSO first light spectrum.jpg
Data from ESPRESSO First Light.

ESPRESSO builds on the foundations laid by the High Accuracy Radial Velocity Planet Searcher (HARPS) instrument at the 3.6-metre telescope at ESO's La Silla Observatory. ESPRESSO benefits not only from the much larger combined light-collecting capacity of the four 8.2-metre VLT Unit Telescopes, but also from improvements in the stability and calibration accuracy that are now possible by laser frequency comb technology. The requirement is to reach 10 cm/s, [5] but the aimed goal is to obtain a precision level of a few cm/s. This would mean a large step forward over current radial-velocity spectrographs like ESO's HARPS. The HARPS instrument can attain a precision of 97 cm/s (3.5 km/h), [6] with an effective precision of the order of 30 cm/s, [7] making it one of only two spectrographs worldwide with such accuracy.[ citation needed ] The ESPRESSO would greatly exceed this capability making detection of Earth-size planets from ground-based instruments possible. Commissioning of ESPRESSO at the VLT started late 2017.

The instrument is capable of operating in 1-UT mode (using one of the telescopes) and in 4-UT mode. In 4-UT mode, in which all the four 8-m telescopes are connected incoherently to form a 16-m equivalent telescope, the spectrograph detects extremely faint objects. [3] [8]

For example, for G2V type stars:

The best-suited candidate stars for ESPRESSO are non-active, non-rotating, quiet G dwarfs to red dwarfs. It operates at the peak of its efficiency for a spectral type up to M4-type stars.

Instrument

First light of the ESPRESSO instrument with all four unit telescopes ESPRESSO instrument achieves first light with all four Unit Telescopes.jpg
First light of the ESPRESSO instrument with all four unit telescopes

For calibration, ESPRESSO uses a laser frequency comb (LFC), with backup of two Th Ar lamps. It features three instrumental modes: singleHR, singleUHR and multiMR [ definition needed ]. In the singleHR mode ESPRESSO can be fed by any of the four UTs. [11]

Status

Engineering rendering of the ESPRESSO instrument Engineering rendering of the ESPRESSO instrument.jpg
Engineering rendering of the ESPRESSO instrument

All design work was completed and finalised by April 2013, with the manufacturing phase of the project commencing thereafter. [1] ESPRESSO was tested on June 3, 2016. [13] ESPRESSO first light occurred on September 25, 2016, during which they spotted various objects, among them the star 60 Sgr A. [14] [15] After being shipped to Chile, installed at the VLT, ESPRESSO saw its first light there on 27 November 2017, in 1-UT mode, observing the star Tau Ceti; [16] [17] [18] the first star observed in the 4-UT mode was on February 3, 2018. [19] [20] [21]

ESPRESSO has been opened to the astronomical community in the 1-UT mode (one single telescope used), and is producing scientific data since October 24, 2018. On quiet stars it has already demonstrated radial-velocity precision of 25 cm/s over a full night. However, there have been some problems, for example, in light collecting efficiency which was around 30% lower than expected and required. And so, some fine-tuning, including replacing the parts causing the efficiency problem and subsequent re-testing, were to be done on the instrument before the full 4-UT mode was open to the scientific community in April 2019. [22] [ needs update ] A problem was discovered in the ESPRESSO charge-coupled device controllers, digital imaging hardware, where a differential nonlinearity issue has reduced the resolution obtainable more severely than was previously feared. The ESO detector team that determined the source of the problem is currently, as of June 2019, working on a new version of the associated hardware in order to remedy this hopefully temporary setback. [23]

On August 29, 2019, the ESPRESSO ETC was updated to reflect the gain in transmission after the technical mission of July. This gain influx was, on average, ≈50% in the UHR and HR modes and ≈40% in the MR. [24]

As of April 6, 2020, the red radial velocity detector has, at least for a very short time, achieved the ≈10  cm/s precision, while the blue detector has so far only managed ≈60  cm/s. [25] Due to the limited spectral coverage and lack of reliability, the Laser Frequency Comb (LFC) is currently not integrated into the telescope and for now complete wavelength calibration will have to rely on the two backup ThAr lamps, with resultant radial velocity measurements values limited by photon noise, stellar jitter and so less precise than expected. [26] The ESPRESSO operator and detector teams are working to characterize and correct the problem, with a dedicated mission expected to take place during 2020. [25]

On May 24, 2020, a team led by A. Suárez Mascareño confirmed the existence of the exoplanet Proxima b, finding it to be about 1.17 times the mass of Earth - smaller than the older estimate of 1.3 times. They also suggested it is located in the habitable zone of its star, which it orbits in 11.2 days. ESPRESSO achieved an accuracy of 26 cm/s, about three times the accuracy obtained with HARPS. They also found a second signal in the data that could be of planetary origin with a semi-amplitude of only 40 cm/s and a 5.15 day period. [27] [28]

On August 28, 2020, it was announced that in the coming weeks minimal science operations are planned to be resumed at the Paranal Observatory, following after a 5-month suspension due to the COVID-19 pandemic. [29] [30]

As of June 11, 2021, there is still an ongoing issue with the blue cryostat detector caused by temperature instabilities, and there has been a communication problem between the Atmospheric Dispersion Corrector and the rest of the instrument, these issues are currently reducing the detection resolution achievable with the instrument. [31]

A major instrument intervention is scheduled between May 1 and May 16, 2022, and the instrument will be out of operations between May 1 until around May 23. After the intervention, an improvement in the overall instrument performance, and in the radial velocity stability, particularly in the blue detector, is expected. [32]

As a result of the instrument intervention the blue cryostat stability has dramatically improved. However, because of a change of the cross dispersion and dispersion direction positions (in both the x and y direction) from the red and blue cryostat detectors induced by the instrument intervention, combining data from different pixels to produce a focused image has become problematic in the MR4x2 mode and the new HR4x2 mode. This problem should be fixed in the new pipeline version, i.e. in an upcoming software update. [33]

Scientific objectives

The main scientific objectives for ESPRESSO are: [34] [35]

Consortium

ESPRESSO is being developed by a consortium consisting on the European Southern Observatory (ESO) and seven scientific institutes:

The principal investigator is Francesco Pepe.

ESPRESSO specifications

ESPRESSO
Telescope VLT (8m)
ScopeRocky planets
Sky aperture 4 arcsec
R≈200.000
λ coverage380 nm-686  nm [36]
λ precision5  m/s
RV stability< 10 cm/s
4-VLT mode (D = 16 m) with RV = 1 m/s
Source: [9] [37] [35]

Radial velocity comparison tables

Planet Mass Distance
AU 		Radial velocity
(vradial)		Note
Jupiter 128.4 m/s
Jupiter 512.7 m/s
Neptune 0.14.8 m/s
Neptune 11.5 m/s
Super-Earth (5 M🜨)0.11.4 m/s
Super-Earth (5 M🜨)10.45 m/s
Earth 0.090.30 m/s
Earth 10.09 m/s
Source: Luca Pasquini, power-point presentation, 2009 [9] Notes: (1) Most precise vradial measurements ever recorded. ESO's HARPS spectrograph was used. [38] [39]
Planets [9]
PlanetPlanet Type
Semimajor Axis
(AU)		Orbital Period
Radial velocity
(m/s)		Detectable by:
51 Pegasi b Hot Jupiter 0.054.23 days55.9 [40] First-generation spectrograph
55 Cancri d Gas giant 5.7714.29 years45.2 [41] First-generation spectrograph
Jupiter Gas giant 5.2011.86 years12.4 [42] First-generation spectrograph
Gliese 581c Super-Earth 0.0712.92 days3.18 [43] Second-generation spectrograph
Saturn Gas giant 9.5829.46 years2.75Second-generation spectrograph
Proxima Centauri b Habitable planet (potentially) 0.0511.19 days1.38 [44] Second-generation spectrograph
Neptune Ice giant 30.10164.79 years0.281Third-generation spectrograph
Earth Habitable planet 1.00365.26 days0.089Third-generation spectrograph (likely)
Pluto Dwarf planet 39.26246.04 years0.00003Not detectable

MK-type stars with planets in the habitable zone

Stellar mass
(M☉)		Planetary mass
(ME)		Lum.
(L0)		Type RHAB
(AU)		 RV
(cm/s)		 Period
(days)
0.101.08×10−4M80.0281686
0.211.07.9×10−3M50.0896521
0.471.06.3×10−2M00.252667
0.651.01.6×10−1K50.4018115
0.782.04.0×10−1K00.6325209
Source: [45] [46]

See also

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References

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  2. ↑ "ESPRESSO". eso.org. Retrieved 8 April 2024.
  3. 1 2 "ESPRESSO - Searching for other Worlds". Centro de Astrofísica da Universidade do Porto. 2010-10-16. Archived from the original on 2010-10-17. Retrieved 2010-10-16.
  4. ↑ "First Light for ESPRESSO — the Next Generation Planet Hunter". www.eso.org. Retrieved 7 December 2017.
  5. ↑ Pepe, F.; Molaro, P.; Cristiani, S.; Rebolo, R.; Santos, N. C.; Dekker, H.; Mégevand, D.; Zerbi, F. M.; Cabral, A.; et al. (January 2014). "ESPRESSO: The next European exoplanet hunter". Astronomische Nachrichten . 335 (1): 8–20. arXiv: 1401.5918 . doi:10.1002/asna.201312004. S2CID   55957013.
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  7. ↑ "ESPRESSO – Searching for other Worlds". Centro de Astrofísica da Universidade do Porto. 16 December 2009. Archived from the original on 17 October 2010. Retrieved 16 October 2010.
  8. ↑ Pepe, Francesco A; Cristiani, Stefano; Rebolo Lopez, Rafael; Santos, Nuno C; et al. (July 2010). "ESPRESSO: the Echelle spectrograph for rocky exoplanets and stable spectroscopic observations" (PDF). In McLean, Ian S; Ramsay, Suzanne K; Takami, Hideki (eds.). Ground-based and Airborne Instrumentation for Astronomy III. Ground-based and Airborne Instrumentation for Astronomy III. Vol. 7735. American Institute of Physics. p. 77350F. Bibcode:2010SPIE.7735E..0FP. doi:10.1117/12.857122 . Retrieved 2013-03-12.
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  11. ↑ Pepe, F.; Molaro, P.; Cristiani, S.; Rebolo, R.; Santos, N. C.; Dekker, H.; Mégevand, D.; Zerbi, F. M.; Cabral, A.; Di Marcantonio, P.; Abreu, M.; Affolter, M.; Aliverti, M.; Allende Prieto, C.; Amate, M.; Avila, G.; Baldini, V.; Bristow, P.; Broeg, C.; Cirami, R.; Coelho, J.; Conconi, P.; Coretti, I.; Cupani, G.; D'Odorico, V.; De Caprio, V.; Delabre, B.; Dorn, R.; Figueira, P.; et al. (2014). "ESPRESSO: The next European exoplanet hunter". arXiv: 1401.5918 [astro-ph.IM].
  12. ↑ "ESO Awards Contracts for Cameras for New Planet Finder". ESO Announcement. Retrieved 8 August 2013.
  13. ↑ "ESPRESSO first laboratory light | espresso". Archived from the original on 2017-08-02. Retrieved 2016-07-08.
  14. ↑ "ESPRESSO Sees Light at the End of the Tunnel - First big step towards adding a new high-resolution spectrograph to the VLT". www.eso.org.
  15. ↑ Ramella, Massimo (October 17, 2016). "ESPRESSO vede la luce in fondo al "tunnel"".
  16. ↑ "ESPRESSO Planet Hunter Heads for Chile". www.eso.org.
  17. ↑ "First light for ESPRESSO—the next generation planet hunter". phys.org.
  18. ↑ Vonarburg, Barbara (2017-12-07). "First light of ESPRESSO". NCCR PlanetS. National Centre of Competence in Research PlanetS. Retrieved 2018-11-07. The first observation was for the star Tau Ceti. It was done using the UT1 of the VLT, the observations made on the four united telescopes will be done later.
  19. ↑ "ESO's VLT Working as 16-metre Telescope for First Time - ESPRESSO instrument achieves first light with all four Unit Telescopes". www.eso.org.
  20. ↑ Bratschi, Pierre (2018-02-14). "ESPRESSO: first time with the 4 UTs of the VLT". NCCR PlanetS. National Centre of Competence in Research PlanetS. Retrieved 2018-11-07. ... first light of ESPRESSO with the four VLT 8.2-meter Unit Telescopes (4UT mode) took place on Saturday February 3rd, 2018... star observed by ESPRESSO with the 4UT mode was the so-called Pepe star
  21. ↑ Echelle SPectrograph for Rocky Exoplanet and Stable Spectroscopic Observations Archived 2017-09-04 at the Wayback Machine , ESO
  22. ↑ Barbara, Vonarburg (2018-11-28). "Fine-tuning Espresso". NCCR PlanetS. National Centre of Competence in Research PlanetS. Retrieved 2018-12-28. ESPRESSO has been opened to the astronomical community and finally started operations on the 24th of October 2018.
  23. ↑ "ESPRESSO News and Press Releases". European Southern Observatory. 2019-06-05. Retrieved 2019-06-21. An issue with the ESPRESSO CCD controllers has recently been identified.
  24. ↑ "ESO - News". www.eso.org. Retrieved 2019-11-12.
  25. 1 2 "ESO - News". www.eso.org. Retrieved 2020-04-11.
  26. ↑ Pepe, F.; et al. (2021). "ESPRESSO at VLT". Astronomy & Astrophysics. 645: A96. arXiv: 2010.00316v1 . doi:10.1051/0004-6361/202038306. S2CID   228854234. A Laser Frequency Comb (LFC) is also available and should have replaced both the ThAr lamp and the Fabry-Pérot (Pasquini& Hubin 2018; Frank et al. 2018; Huke et al. 2018), but, due to lack of reliability and limited spectral coverage, it is currently not integrated in the operational scheme ... This situation might compromize the ability of ESPRESSO of guaranteeing RV repeatability at the 10 cm s−1 level over years.
  27. ↑ Suárez Mascareño, A.; Faria, J. P.; Figueira, P.; Lovis, C.; Damasso, M.; González Hernández, J. I.; Rebolo, R.; Cristiano, S.; Pepe, F.; Santos, N. C.; Zapatero Osorio, M. R.; Adibekyan, V.; Hojjatpanah, S.; Sozzetti, A.; Murgas, F.; Abreo, M.; Affolter, M.; Alibert, Y.; Aliverti, M.; Allart, R.; Allende Prieto, C.; Alves, D.; Amate, M.; Avila, G.; Baldini, V.; Bandi, T.; Barros, S. C. C.; Bianco, A.; Benz, W.; et al. (2020). "Revisiting Proxima with ESPRESSO". Astronomy & Astrophysics. 639: A77. arXiv: 2005.12114 . Bibcode:2020A&A...639A..77S. doi:10.1051/0004-6361/202037745. S2CID   218869742.
  28. ↑ Revisiting Proxima with ESPRESSO
  29. ↑ "Minimal Science Operations to be Resumed at Paranal, APEX and La Silla". www.eso.org. Retrieved 2020-09-07.
  30. ↑ "ann20010 — Announcement COVID-19 coronavirus measures at ESO" . Retrieved 2020-09-07.
  31. ↑ "ESO - News". www.eso.org. Retrieved 2022-04-22. Detailed Description
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  33. ↑ "ESO - News". www.eso.org. Retrieved 2023-01-28. Detailed Description
  34. ↑ ESPRESSO - A VLT Project Archived 2016-09-25 at the Wayback Machine . Accessed 12 October 2017.
  35. 1 2 ESPRESSO Baseline Specification. European Southern Observatory (ESO). Accessed: 12 October 2017
  36. ↑ ESPRESSO Archived 2017-09-04 at the Wayback Machine . ESO.
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  40. ↑ "51 Peg b". Exoplanets Data Explorer.
  41. ↑ "55 Cnc d". Exoplanets Data Explorer.
  42. ↑ Endl, Michael. "The Doppler Method, or Radial Velocity Detection of Planets" (.ppt). University of Texas at Austin. Retrieved 6 October 2020. (pdf version)
  43. ↑ "GJ 581 c". Exoplanets Data Explorer.
  44. ↑ "Proxima Cen b". Extrasolar Planets Encyclopaedia . 2024.
  45. ↑ "An NIR laser frequency comb for high precision Doppler planet surveys". Chinese Academy of Sciences. 2010-10-16. Retrieved 2010-10-16.[ dead link ]
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