Orbiting – Enabling Meaningful Connections\n\n\n\n\n\nMeet new People, Make New Friends, and Build Communities

Orbiting

Transcendence Volume I, Book 1: Introduction

Discussing the Impact of Our Exoplanet Study: How This Impacts Everything

This paper is available on arxiv under CC 4.0 license. Authors: (1) Andrew Ridden-Harper, Department of Astronomy and Carl Sagan Institute, Cornell University & Las Cumbres Observatory; (2) Stevanus K. Nugroho, Astrobiology Center & Japan & National Astronomical Observatory of Japan; (3) Laura Flagg, Department of Astronomy and Carl Sagan Institute, Cornell University; (4) Ray Jayawardhana, Department of Astronomy, Cornell University; (5) Jake D. Turner, Department of Astronomy and Carl Sagan Institute, Cornell University & NHFP Sagan Fellow; (6) Ernst de Mooij, Astrophysics Research Centre, School of Mathematics and Physics & Queen’s University Belfast; (7) Ryan MacDonald, Department of Astronomy and Carl Sagan Institute; (8) Emily Deibert, David A. Dunlap Department of Astronomy & Astrophysics, University of Toronto & Gemini Observatory, NSF’s NOIRLab; (9) Motohide Tamura, Dunlap Institute for Astronomy & Astrophysics, University of Toronto (10) Takayuki Kotani, Department of Astronomy, Graduate School of Science, The University of Tokyo, Astrobiology Center & National Astronomical Observatory of Japan; (11) Teruyuki Hirano, Astrobiology Center, National Astronomical Observatory of Japan & Department of Astronomical Science, The Graduate University for Advanced Studies; (12) Masayuki Kuzuhara, Las Cumbres Observatory & Astrobiology Center; (13) Masashi Omiya, Las Cumbres Observatory & Astrobiology Center; (14) Nobuhiko Kusakabe, Las Cumbres Observatory & Astrobiology Center. Table of Links Abstract & Introduction Observation Data Reduction and Processing Model Spectra Cross-Correlation Method Results Clouds and Hazes Implications for JWST Conclusion and Acknowledgement Appendix & References ABSTRACT Terrestrial exoplanets orbiting M-dwarf stars are promising targets for transmission spectroscopy with existing or near-future instrumentation. The atmospheric composition of such rocky planets remains an open question, especially given the high X-ray and ultraviolet flux from their host M dwarfs that can drive atmospheric escape. The 1.3 R⊕ exoplanet GJ 486b (Teq ∼ 700 K), orbiting an M3.5 star, is expected to have one of the strongest transmission spectroscopy signals among known terrestrial exoplanets. We observed three transits of GJ 486b using three different high-resolution spectrographs: IRD on Subaru, IGRINS on Gemini-South, and SPIRou on the Canada-France-Hawai’i Telescope. We searched for atmospheric absorption from a wide variety of molecular species via the cross-correlation method, but did not detect any robust atmospheric signals. Nevertheless, our observations are sufficiently sensitive to rule out several clear atmospheric scenarios via injection and recovery tests, and extend comparative exoplanetology into the terrestrial regime. Our results suggest that GJ 486b does not possess a clear H2/He-dominated atmosphere, nor a clear 100% water-vapor atmosphere. Other secondary atmospheres with high mean molecular weights or H2/He-dominated atmospheres with clouds remain possible. Our findings provide further evidence suggesting that terrestrial planets orbiting M-dwarf stars may experience significant atmospheric loss. : Exoplanet atmospheres (487) — Planetary atmospheres (1244) — Exoplanets (498) — Exoplanet atmospheric composition (2021) Keywords 1. INTRODUCTION Exoplanets that transit M-dwarf stars produce relatively deep transits due to their high planet-star radius ratios. Consequently, it may be possible to detect biosignatures in the atmospheres of terrestrial exoplanets with existing or near-future instrumentation (e.g., Snellen et al. 2013; Wunderlich et al. 2019). However, the long-term habitability of such planets depends crucially on the stability of their atmospheres, which are subject to high X-ray + extreme UV (XUV) emissions during the pre-main-sequence phase of their M-dwarf hosts (e.g., Shkolnik & Barman 2014; Peacock et al. 2020) as well as flare events (e.g., Neves Ribeiro do Amaral et al. 2022) that can drive atmospheric escape (e.g., Vidal-Madjar et al. 2003; Bourrier et al. 2017a; Airapetian et al. 2017). Terrestrial exoplanets are expected to exhibit a rich diversity in atmospheric compositions. Exoplanets with Rp < 1.4 R⊕ and orbital periods < 100 days likely form as gas-rich sub-Neptunes that subsequently lose their primordial atmospheres due to photoevaporation (Rogers & Owen 2021). The amount of primordial atmosphere retained depends on several factors, such as their host star’s spectral energy distribution and activity levels, along with how much gas they accrete during formation (e.g., Bolmont et al. 2017; Owen et al. 2020). Should the primordial hydrogen-dominated atmosphere be lost, a secondary atmosphere may be retained. The composition of secondary atmospheres depends on a variety of processes, including interior outgassing, impact delivery, erosion, atmosphere-surface exchange, weathering, and volatile sequestration (e.g., Rogers et al. 2011). Driven by these processes, hot terrestrial planets (T & 1500 K) are predicted to have atmospheres containing atoms and ions, such as Na or Ca+, produced by surface vaporization (Schaefer & Fegley 2009) — though other hydrogen- or nitrogen-rich compositions are possible (Miguel 2019). However, cooler terrestrial planets are likely rich in molecular species, such as H2O, CO2, CO, O2, C2H2, and CH4 (e.g., Ramirez & Kaltenegger 2014; Madhusudhan et al. 2016; Kite & Schaefer 2021). Given the range of theoretical possibilities, observational constraints on the composition of terrestrial exoplanet atmospheres are crucially needed. While there have been several attempts to detect the atmospheres of a few terrestrial exoplanets, these have only yielded constraints from nondetections. For example, 55 Cancri e is a 1.9 R⊕ exoplanet with a temperature of approximately 2400 K due to its 17 hr orbit around its G8V host star (Morris et al. 2021). Hubble Space Telescope observations suggest that 55 Cancri e may possess a thick atmosphere (Tsiaras et al. 2016). However, phase curve observations with the Spitzer space telescope (Demory et al. 2016) and ground-based high-resolution transmission spectroscopy point toward 55 Cancri e not possessing a thick atmosphere or having no atmosphere at all (Ridden-Harper et al. 2016; Esteves et al. 2017; Jindal et al. 2020; Deibert et al. 2021a; Zhang et al. 2021). A similar result was found for the cooler 1.3 R⊕ exoplanet LHS 3844 b, which has an equilibrium temperature of 800 K and orbits an M5 host star (Vanderspek et al. 2019). Kreidberg et al. (2019) observed the phase curve of LHS 3844 b with the Spitzer space telescope and found that thick atmospheres with surface pressures greater than 10 bar could be ruled out, while less massive atmospheres would be susceptible to erosion by the stellar wind. Additionally, they found that a bare rock model fit their data well. Another candidate for atmospheric characterization that orbits an M-dwarf is GJ 1132b, which has a radius, mass, and equilibrium temperature of 1.1 R⊕, 1.7 M⊕, and 580 K, respectively (Berta-Thompson et al. 2015). Using transit observations from the Hubble Space Telescope (HST), Swain et al. (2021) inferred that GJ 1132b possesses a H/He-rich atmosphere with large-amplitude spectral features. However, using the same HST data, Libby-Roberts et al. (2022) and Mugnai et al. (2021) independently found a featureless transmission spectrum, possibly indicating an atmosphere with a high mean molecular weight (MMW), a high-altitude aerosol layer, or a near-total lack of an atmosphere. These contrasting results highlight the difficulty of characterizing the atmospheres of small planets, even with space-based instrumentation. Comprehensive searches for the atmospheres of the seven approximately Earth-sized planets that transit the M8V star TRAPPIST-1 have also been carried out. These transit observations with the Hubble and Spitzer space telescopes all point toward the absence of extended hydrogen-dominated atmospheres. However, denser, potentially habitable atmospheres are consistent with the observational limits for some TRAPPIST-1 planets (de Wit et al. 2016; Bourrier et al. 2017b,a; de Wit et al. 2018; Zhang et al. 2018; Wakeford et al. 2019; Gressier et al. 2022). GJ 486b[1] is a 1.3 R⊕ and 2.8 M⊕ exoplanet with an equilibrium temperature of about 700 K, an M3.5 V host star of J-band magnitude 7.2, and an orbital period of 1.5 days (Trifonov et al. 2021). These system properties make GJ 486b well suited to atmospheric characterization with transmission spectroscopy, as reflected by it having one of the largest transmission spectroscopy metrics (as defined by Kempton et al. 2018) of all known terrestrial planets (Trifonov et al. 2021). Therefore, GJ 486b is an ideal observational target to inform our understanding of terrestrial planets around M-dwarf stars. Previous studies have surmised that a wide range of atmospheric compositions are possible for GJ 486b. Caballero et al. (2022) refined GJ 486b’s mass and radius, and presented a suite of interior and atmospheric models. They showed that possible atmospheres include: (i) a H/He-dominated atmosphere with solar abundances; (ii) a H/He atmosphere with enhanced metallicity (e.g., 100x solar abundances); (iii) a H2O-dominated atmosphere; (iv) a CO2-dominated atmosphere; or (v) bare rock with a tenuous atmosphere, possibly containing Na. Geochemical models based on initial conditions representative of a range of possible planets suggest that a H2O-dominated atmosphere is the most likely outcome for a 3 M⊕ planet like GJ 486b (Ortenzi et al. 2020). However, carbonaceous chondrite outgassing measurements suggest that CO2-dominated atmospheres could also evolve on terrestrial planets (Thompson et al. 2021). Differentiating between these scenarios requires spectroscopic observations. Molecular species such as those expected to be in GJ 486b’s atmosphere produce dense forests of spectral lines that can be individually resolved with high-resolution spectroscopy. The signals from these lines can be combined, even if they are individually hidden in the noise, by cross-correlating the data with a template containing the molecular lines (e.g., Snellen et al. 2010; Birkby 2018). This powerful technique has facilitated the detection of species such as H2O, CO, HCN, CH4, NH3, and C2H2 in the transmission spectra of hot Jupiters (e.g., Giacobbe et al. 2021). As high-resolution spectroscopy probes line cores, which contain information about the upper (low-pressure) regions of exoplanet atmospheres, it is highly complementary to low-resolution observations from telescopes such as the JWST, which probe higher pressures (Brogi & Line 2019). JWST is scheduled to observe two transits and eclipses of GJ 486b in programs GO 1981[2] (P.I.: K. Stevenson) and GO 1743[3] (P. I.: M. Mansfield), respectively. Here, we present the first high-resolution transmission spectroscopy observations of GJ 486b. We use three transits to constrain GJ 486b’s atmospheric composition. In what follows, in Sections 2 and 3 we describe our observations and data reduction approach. Section 4 describes our model spectra, while Section 5 describes our cross-correlation methodology. Section 6 presents our results, while Section 8 discusses the implications of our results for the upcoming JWST observations. Finally, Section 9 offers concluding remarks. [1] Alternative names include Wolf 437b and TOI 1827b. [2] program-information.html?id=1981 https://www.stsci.edu/jwst/science-execution/ [3] program-information.html?id=1743 https://www.stsci.edu/jwst/science-execution/

High-Resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b: Abstract & Intro

This paper is available on arxiv under CC 4.0 license. Authors: (1) Andrew Ridden-Harper, Department of Astronomy and Carl Sagan Institute, Cornell University & Las Cumbres Observatory; (2) Stevanus K. Nugroho, Astrobiology Center & Japan & National Astronomical Observatory of Japan; (3) Laura Flagg, Department of Astronomy and Carl Sagan Institute, Cornell University; (4) Ray Jayawardhana, Department of Astronomy, Cornell University; (5) Jake D. Turner, Department of Astronomy and Carl Sagan Institute, Cornell University & NHFP Sagan Fellow; (6) Ernst de Mooij, Astrophysics Research Centre, School of Mathematics and Physics & Queen’s University Belfast; (7) Ryan MacDonald, Department of Astronomy and Carl Sagan Institute; (8) Emily Deibert, David A. Dunlap Department of Astronomy & Astrophysics, University of Toronto & Gemini Observatory, NSF’s NOIRLab; (9) Motohide Tamura, Dunlap Institute for Astronomy & Astrophysics, University of Toronto (10) Takayuki Kotani, Department of Astronomy, Graduate School of Science, The University of Tokyo, Astrobiology Center & National Astronomical Observatory of Japan; (11) Teruyuki Hirano, Astrobiology Center, National Astronomical Observatory of Japan & Department of Astronomical Science, The Graduate University for Advanced Studies; (12) Masayuki Kuzuhara, Las Cumbres Observatory & Astrobiology Center; (13) Masashi Omiya, Las Cumbres Observatory & Astrobiology Center; (14) Nobuhiko Kusakabe, Las Cumbres Observatory & Astrobiology Center. Table of Links Abstract & Introduction Observation Data Reduction and Processing Model Spectra Cross-Correlation Method Results Clouds and Hazes Implications for JWST Conclusion and Acknowledgement Appendix & References 9. CONCLUSION In this study, we searched for the atmosphere of the 1.3 R⊕ exoplanet GJ 486b using high-resolution transmission spectroscopy. Our resultant atmospheric constraints additionally offer an improved understanding of the possible atmospheres for terrestrial planets orbiting M-dwarf stars. We observed three transits of GJ 486b with the spectrographs IRD, IGRINS, and SPIRou, and searched for absorption by its atmosphere with the high-resolution cross-correlation method. We searched for C2H2, CH4, CO, CO2, FeH, H2O, HCN, H2S, K, Na, NH3, PH3, SiO, TiO, and VO, but did not detect any robust atmospheric signals. Our best potential detection was H2O at the 3σ level, seen only in the IGRINS data set. However, this potential signal is likely an artifact of imperfectly removed H2O lines in the stellar spectrum. We suggest that it may be possible to improve the suppression of these stellar lines by using 3D models of stellar convection, as shown by Chiavassa & Brogi (2019). Nevertheless, we derived informative upper limits on the abundances of many chemical species by performing signal injection and recovery tests. Our recovery tests allow us to rule out a clear H2/He-dominated atmosphere with solar molecular abundances to a confidence of >5σ, while also ruling out a clear 100% water atmosphere to a confidence of 3σ. Since a water-dominated atmosphere is often considered to be the most likely possibility for 3 M⊕ planets like GJ 486b (e.g., Ortenzi et al. 2020), our results could have important implications for planetary interior models. We also investigated the implications of our findings for the upcoming JWST transit observations of GJ 486b. We found that these observations will be especially sensitive to the presence of CO2, but with weaker sensitivity to H2O, highlighting the complementary capabilities of high-resolution and JWST observations. In summary, our results indicate that GJ 486b does not possess a cloud-free H/He-dominated atmosphere that has solar abundances. However, it may possess a secondary atmosphere with high mean molecular weight or a H2/He-dominated atmosphere with clouds. Our findings provide further evidence suggesting that terrestrial planets orbiting M-dwarf stars experience significant atmospheric loss. ACKNOWLEDGMENTS We thank the anonymous reviewer for constructive comments. We are also grateful to Hajime Kawahara for helpful suggestions. This research is based [in part] on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We are honored and grateful for the opportunity of observing the Universe from Maunakea, which has cultural, historical, and natural significance in Hawaii. This work used the Immersion Grating Infrared Spectrometer (IGRINS) that was developed under a collaboration between the University of Texas at Austin and the Korea Astronomy and Space Science Institute (KASI) with the financial support of the Mt. Cuba Astronomical Foundation, of the US National Science Foundation under grants AST-1229522 and AST-1702267, of the McDonald Observatory of the University of Texas at Austin, of the Korean GMT Project of KASI, and of the Gemini Observatory. Based on observations obtained at the international Gemini Observatory, a program of NSF’s NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), the National Research Council (Canada), Agencia Nacional de Investigaci´on y Desarrollo (Chile), Ministerio de Ciencia, Tecnolog´ıa e Innovaci´on (Argentina), Minist´erio da Ciˆencia, Tecnologia, Inova¸c˜oes e Comunica¸c˜oes (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). Based on observations obtained at the CanadaFrance-Hawaii Telescope (CFHT), which is operated from the summit of Maunakea by the National Research Council of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. The observations at the Canada-France-Hawaii Telescope were performed with care and respect from the summit of Maunakea which is a significant cultural and historic site. Based on observations obtained with SPIRou, an international project led by Institut de Recherche en Astrophysique et Plan´etologie, Toulouse, France. This research has made use of the Extrasolar Planet Encyclopaedia, NASA’s Astrophysics Data System Bibliographic Services, and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. M.T. is supported by JSPS KAKENHI grant Nos. 18H05442, 15H02063, and 22000005. S. K. N. is supported by JSPS KAKENHI grant No. 22K14092. J.D.T’s support for this work was provided by NASA through the NASA Hubble Fellowship grant #HSTHF2-51495.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5- 26555. : 8.2 m Subaru telescope (IRD), 8.1 m Gemini-South telescope (IGRINS), 3.6 m Canada France Hawai’i Telescope (SPIRou) Facilities : Astropy (Astropy Collaboration et al. 2013, 2018); SciPy (Virtanen et al. 2020); NumPy (Harris et al. 2020); petitRADTRANS (Molli`ere et al. 2019); SpectRes (Carnall 2017). Software

High-Resolution Transmission Spectroscopy: Conclusion and Acknowledgement

This paper is under CC 4.0 license. available on arxiv Authors: (1) Prajwal Niraula, Department of Earth, Atmospheric and Planetary Sciences; (2) Julien de Wit, Department of Earth, Atmospheric and Planetary Sciences; (3) Benjamin V. Rackham, Department of Earth, Atmospheric and Planetary Sciences; (4) Elsa Ducrot, Astrobiology Research Unit, University of Li`ege; (5) Artem Burdanov, Department of Earth, Atmospheric and Planetary Sciences; (6) Ian J. M. Crossfield, Kansas University Department of Physics and Astronomy; (7) Valerie Van Grootel´, Space Sciences, Technologies and Astrophysics Research (STAR) Institute, University of Li`ege; (8) Catriona Murray, 5Cavendish Laboratory; (9) Lionel J. Garcia, Astrobiology Research Unit, University of Li`ege; (10) Roi Alonso, Instituto de Astrof´ısica de Canarias & Dpto. de Astrof´ısica, Universidad de La Laguna; (11) Corey Beard, Department of Physics & Astronomy, The University of California; (12) Yilen Gomez Maqueo Chew, Instituto de Astronom´ıa, Universidad Nacional Aut´onoma de M´exico, Ciudad Universitaria; (13) Laetitia Delrez, Astrobiology Research Unit, University of Li`ege, Space Sciences, Technologies and Astrophysics Research (STAR) Institute, University of Li`ege & 0Observatoire de lUniversit´e de Gen`eve; (14) Brice-Olivier Demory, University of Bern, Center for Space and Habitability; (15) Benjamin J. Fulton, NASA Exoplanet Science Institute/Caltech-IPAC; (16) Michael Gillon, Astrobiology Research Unit, University of Li`ege; (17) Maximilian N. Gunther, Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology; (18) Andrew W. Howard, California Institute of Technology; (19) Howard Issacson, Department of Astronomy, University of California Berkeley; (20) Emmanuel Jehin, Space Sciences, Technologies and Astrophysics Research (STAR) Institute, University of Li`ege; (21) Peter P. Pedersen, Cavendish Laboratory; (22) Francisco J. Pozuelos, Astrobiology Research Unit, University of Li`ege & Space Sciences, Technologies and Astrophysics Research (STAR) Institute, University of Li`ege; (23) Didier Queloz, Cavendish Laboratory; (24) Rafael Rebolo-Lopez, Instituto de Astrof´ısica de Canarias & Dpto. de Astrof´ısica, Universidad de La Laguna'; (25) Sairam Lalitha, School of Physics & Astronomy, University of Birmingham; (26) Daniel Sebastian, Astrobiology Research Unit, University of Li`ege (27) Samantha Thompson, Cavendish Laboratory; (28) Amaury H.M.J. Triaud, School of Physics & Astronomy, University of Birmingham. Table of Links Abstract & Introduction Observation Analysis and Validation Future Prospects & References ABSTRACT We report on the discovery of a transiting Earth-sized (0.95R⊕) planet around an M3.5 dwarf star at 57 pc, K2-315b. The planet has a period of ∼3.14 days, i.e. ∼π, with an instellation of 7.45 S⊕. The detection was made using publicly available data from K2’s Campaign 15. We observed three additional transits with SPECULOOS Southern and Northern Observatories, and a stellar spectrum from Keck/HIRES, which allowed us to validate the planetary nature of the signal. The confirmed planet is well suited for comparative terrestrial exoplanetology. While exoplanets transiting ultracool dwarfs present the best opportunity for atmospheric studies of terrestrial exoplanets with the James Webb Space Telescope, those orbiting mid-M dwarfs within 100 pc such as K2-315b will become increasingly accessible with the next generation of observatories. stars: individual (2MASS J15120519-2006307, EPIC 249631677, TIC 70298662, K2-315b) – planets and satellites: detection Keywords: 1. INTRODUCTION The redesigned Kepler mission, K2 (Howell et al. 2014), has been a success by adding almost 400 confirmed planets to the 2,348 discovered by the original mission[1]. Building upon Kepler (Borucki et al. 2010), K2 expanded the search of planets around brighter stars, covered a wider region of sky along the ecliptic, and studied a variety of astronomical objects . Together, these endeavors have revolutionized the field of exoplanetary science by quadrupling the number of exoplanets known at the time, while K2 in particular has led to exciting discoveries, such as disintegrating planetesimals around the white dwarf WD-1145 (Vanderburg et al. 2015), multi-planet systems around bright stars like GJ 9827 (K2-135) (Niraula et al. 2017; Rodriguez et al. 2018), and resonant chains of planets like the K2-138 system with five planets (Christiansen et al. 2018). Space-based platforms such as Kepler can provide high-quality continuous monitoring of targets above the Earth’s atmosphere. The simultaneous photometric monitoring of tens of thousands of stars enables finding rare configurations (e.g., WD-1145) and answering science questions regarding planetary populations that are more statistical in nature such as how unique our own Solar System is, or what are the most common type of planets (e.g. Fressin et al. 2013; Fulton et al. 2017). Ground-based facilities, on the other hand, often detect fewer planets while operating at a lower cost. These planets frequently exhibit larger signal-to-noise ratios (SNRs) in various metrics (e.g., transmission), thereby allowing for these planets to be characterized further. One such example is the TRAPPIST-1 planetary system (Gillon et al. 2016, 2017), discovered by the TRAPPISTUltra Cool Dwarf Transiting Survey, a prototype survey for the SPECULOOS Survey (Gillon et al. 2013). The goal of the SPECULOOS Survey is to explore the nearest ultracool dwarfs (Teff <3000 K) for transits of rocky planets (Burdanov et al. 2018; Delrez et al. 2018; Jehin et al. 2018; Sebastian et al. in prep.). Although few systems are expected (Delrez et al. 2018; Sebastian et al. in prep.), their impact on the field will be significant as they should provide most of the temperate Earthsized exoplanets amenable for atmospheric studies with the next generation of observatories such as JWST (e.g. Gillon et al. 2020). Beyond the SPECULOOS Survey, which monitors nearby late-M dwarfs for terrestrial planets, the SPECULOOS telescopes have been used to study the planetary population around mid- and late-M dwarfs. In that context, SPECULOOS facilities have been involved in following up and validating planetary candidates, notably from TESS (G¨unther et al. 2019; Kostov et al. 2019; Quinn et al. 2019). Next to confirming planetary candidates that cross detection thresholds, we have started to investigate weaker signals. For this work, we revisited K2 data, a mission which ended only in 2019. We reanalyzed the light curves of stars with Teff < 3500 K, a Kepler magnitude < 15, and a log g > 4.5. While these criteria were motivated particularly to look for planets around ultra-cool dwarfs, they were relaxed in order to allow room for errors in the stellar properties and improve completeness of the analysis. Among the 1,213 stars fitting these criteria, EPIC 249631677 presented the strongest periodic transit-like signal. In this paper, we report the discovery of an Earthsized K2 planet in a close-in orbit around EPIC 249631677. The paper is structured as follow; observations (Section 2), analysis and validation (Section 3), and the discussion in regards to future prospects for characterization (Section 4). In this paper, we report the discovery of an Earthsized K2 planet in a close-in orbit around EPIC 249631677. The paper is structured as follow; observations (Section 2), analysis and validation (Section 3), and the discussion in regards to future prospects for characterization (Section 4). [1] https://exoplanetarchive.ipac.caltech.edu

π Earth: a 3.14-day Earth-sized Planet from K2's Kitchen Served Warm: Abstract & Intro

Lasers by Hal Hellman, is part of the HackerNoon Books Series. You can jump to any chapter in this book . COMMUNICATIONS here COMMUNICATIONS Future deep space missions are expected to require extremely high data transmission rates (on the order of a million bits per second) to relay the huge quantities of scientific and engineering information gathered by the spacecraft. Higher data rates are necessary to increase both the total capacity and the speed of transmission. By comparison, the Mariner-4 spacecraft that sent back TV pictures of Mars had a data rate of only eight bits per second—a hundred thousand times too small for future missions. The use of lasers would mean that results could be transmitted to earth in seconds instead of the 8 hours it took for the photos to be sent from Mariner-4. One of the problems to be solved in using lasers for deep space communication, oddly enough, is that of pointing accuracy. Since the beam of laser energy is narrow, it would be possible for the radiation to miss the earth altogether and be lost entirely unless the laser were pointed at the receiver with extreme precision. Aiming a gun at a target 50 yards away is one thing; aiming a laser from an unmanned spacecraft 100 million miles away is quite another. It is believed, however, that present techniques can cope with the problem. Another peculiarity of laser communication is that it will probably be accomplished faster and more readily in space than here on earth. Powerful though laser light may be, it is light and is therefore impeded to some extent by our atmosphere even under good conditions. Data transmissions of 20 and 30 miles have already been accomplished in good weather with lasers. But if you have ever tried to force a searchlight beam or shine automobile headlights through heavy fog, rain, or snow, you will appreciate the magnitude of the problem under these conditions. The use of infrared frequencies helps to some extent, since infrared is somewhat more penetrating, but the poor-weather problem is a serious one. A possible solution is the use of “light pipes”, similar to the wave guides already in use for certain microwave applications over short distances. But as often happens, new developments create new needs; how, for example, can we get the laser beam to stay centered in the pipe and follow curves? A series of closely spaced lenses, about 1000 per mile, probably would accomplish this, but too much light would be lost by scattering from the many lens surfaces. Scientists are experimenting with a new kind of “lens”, one that uses variations in the density of gases to focus and guide the beam automatically. Since there are no surfaces in the path of the light beam, and since the gas is transparent and free of turbulence, the laser beam is not appreciably weakened or scattered as it travels through the pipe. Figure 31 Laser light beam being guided through a “light pipe” by a gas “lens”. Heating coil (lower left) or mixture of gases (lower right) are two possible ways of maintaining proper density gradient in the gas. shows how the gas focusing principle might be used to guide a beam through a curving pipe. The shading represents the density of the gas. Several means have been developed to keep the gas denser in the center than around the outside. When the pipe curves, the light beam starts moving off the axis of the pipe. The gas then acts like a prism, deflecting the light beam in the direction of the curvature of the “prism”. Figure 31 In communication between distant space and earth, a light pipe might be a little cumbersome; hence it may prove necessary to set up an intermediate orbiting relay station that will, particularly in cases of poor weather, intercept the incoming laser beam and convert it to radio frequencies that can penetrate our atmosphere with greater reliability. Powering space-borne lasers will, of course, be a problem. Indeed one of the major unsolved problems in production of spacecraft and long-term satellites is the provision of an adequate supply of power. Fuel cells and solar cells have helped but do not give the whole answer. One other approach has already been developed: a sun-pumped laser. Sunlight focused onto the side of the laser (see ) provides the pumping power, enabling the device to put out 1 watt of continuous infrared radiation, enough for special space applications. Descendents of this device could produce visible light if this is deemed desirable. Figure 32 Another approach, using , is even more intriguing and may have greater consequences. Chemical lasers will derive their energy from their internal chemistry rather than from the outside. A mixture of two chemicals may be all that is needed to initiate laser action aboard a spacecraft or satellite. (Chemical lasers also offer the promise of even greater concentrations of power than have been achieved heretofore, which may make them useful in plasma research.) chemical lasers With all these possibilities, it may still be that spacecraft will need more power than is available on board. The narrow beam of the laser offers one more fascinating possibility, especially in the case of satellites relatively near earth. The light of a laser might actually be used to beam energy to a receiver, either for immediate use or storage. It would then become possible to “refuel” satellites at will, giving them much greater capabilities. If available laser power is great enough, laser beams might even be used to push satellites back into their proper orbits when they begin to wander off course, as they almost invariably do after a while. Figure 32 Artist’s rendering of sun-pumped laser as it would operate in space. The sun’s rays are collected by a parabolic reflector and are focused on the laser’s surface by two cylindrical mirrors. Sun Parabolic Collector Hyperbolic-cylindric secondary mirror Semi-circular-cylindric tertiary mirror Laser beam About HackerNoon Book Series: We bring you the most important technical, scientific, and insightful public domain books. This book is part of the public domain. Hal Hellman (2021). Laser. Urbana, Illinois: Project Gutenberg. Retrieved October 2022 https://www.gutenberg.org/cache/epub/65512/pg65512-images.html This eBook is for the use of anyone anywhere at no cost and with almost no restrictions whatsoever. You may copy it, give it away or re-use it under the terms of the Project Gutenberg License included with this eBook or online at , located at . www.gutenberg.org https://www.gutenberg.org/policy/license.html

Future deep space missions are expected to require extremely high data transmission rates

Space exploration has captivated the human imagination for centuries. It has helped to drive us to venture beyond our living planet to uncover the mysteries of the cosmos. Today, we are in the modern era with the fascinating world of From the first space mission (which was once a matter of imagination) to the present reality of humans walking on the lunar surface and satellites orbiting distant planets, the advancement of technology is undeniable. Mars, in particular, has become a focus of exploration with robotic missions like the Curiosity rover, Perseverance rover, Ingenuity helicopter, and Zhurong rover actively operating on its surface and sending data to Earth. They are equipped with ) with the capability of analyzing the samples. space exploration. machine learning(ML Missions and explorations are not just limited to Mars, other planets, and their natural satellites. Researchers are still working hard to uncover more of this universe’s mysteries. Some interesting strides, in recent times, are as follows: The first-ever detection of , gravitational waves First ever image of a , Black Hole The deepest, sharpest infrared view of from NASA's James Webb Space Telescope, and many more. the universe to date For these achievements, AI and ML have assisted to some extent but advanced use in space missions is yet to be realized. AI The revelation of water activities on Mars has further boosted our curiosity about the possibility of life beyond Earth. Despite the high cost and technological challenges, the idea of sending human missions to Mars and other planets is a tantalizing prospect, and this is where AI could play a pivotal role in shaping the future of space exploration. This article aims to dive into various aspects related to space exploration in this context. The views and opinions expressed in this article are solely those of the author and do not necessarily reflect the official policy or position of any space agency or organization. Disclaimer: Here are some of the ways that AI is being used in space today: AI is being used to develop autonomous navigation systems for spacecraft. These systems can navigate spacecraft without human intervention so they can reduce the risk of accidents and improve efficiency. AI-powered navigation systems are very useful for guiding spacecraft and rovers with precision. For example; NASA's Mars rovers Curiosity and Perseverance. These rovers utilize AI algorithms to process images, analyze terrain, and autonomously plan routes to avoid obstacles while efficiently reaching their intended destinations. In addition, NASA developed an system to map the moon virtually in 2018. 🚀Autonomous navigation: AI-enabled navigation AI is being used to manage resources in space like fuel and food. AI-powered systems can optimize the use of these resources which can help to extend the lifespan of missions and reduce costs. For example, some satellites need regular power consumption to operate correctly whereas AI is playing a crucial role to manage the power and other resources. 🚀Resource management: AI is being used to analyze data from space missions. This data can be used to learn more about the universe, identify potential hazards, and improve the design of future missions. The vast amount of data collected from telescopes, satellites, and space probes need advanced AI tools for efficient analysis. Machine Learning(ML) algorithms assist in sifting through massive datasets to identify patterns and scientifically relevant information. It can accelerate the process of discovering new celestial bodies, understanding cosmic phenomena, and uncovering insights into the universe's evolution. For example, NASA uses as a helpful assistant for creating Earth observation satellite systems. 🚀Data analysis: Daphne Currently, AI processes a large amount of images or data every minute. It assists to predict the planet’s surfaces or geological conditions. In our living planet’s cases, AI assists to forecast the weather or other space-related images by analyzing the captured images. 🚀Enhances satellite imagery: NASA to facilitate the discovery of exoplanets through the Kepler Telescope. One notable example is the use of a convolutional neural network (CNN) called AstroNet K2. This AI system was designed to analyze signals from the Kepler Telescope. By training AstroNet K2 to an accuracy rate of 98%, NASA successfully identified new exoplanets like Kepler 80g and Kepler 90i. 🚀Exoplanet discovery: utilized AI AI is being used to assess the risks associated with space missions. This can help to identify potential problems and develop mitigation strategies. In the environment of space, equipment failures can have very tough consequences. AI-driven predictive maintenance helps detect potential faults by analyzing sensor data and predicting when components might fail. This capability enables astronauts and mission control to take preemptive actions to prevent catastrophic failures and ensure the safety of both crewed and uncrewed missions. 🚀Risk assessment, Fault Detection, and Mitigation: You know space missions are generally a very complicated and difficult process that involves various steps and technologies so a single mistake might cause significant losses. AI is being used to make decisions about space missions to ensure that missions are conducted safely and efficiently so that it reduces the risks caused due to human error. 🚀Decision-making: These are just a few of the ways that AI is being used in space today. As AI continues to evolve, we can expect to see even more innovative and groundbreaking applications of this technology in the years to come. AI for Space Exploration: Current Situation : NASA's AI Exploration Initiative NASA is actively engaged in a multi-year effort known as the AI Exploration Initiative. This initiative's primary objective is to advance and implement AI technologies within the realm of space exploration. It centers around four key focal points: autonomous systems, data science, human-AI collaboration, and risk evaluation. ESA’s Program for Artificial Intelligence in Space Exploration (ARTES): The ARTES program, initiated by the European Space Agency constitutes a series of activities dedicated to the development and application of AI technologies in the context of space exploration. This program concentrates on four principal domains: autonomous systems, robotics, data analysis, and risk assessment. : The Deep Space Atomic Clock (DSAC) Project The DSAC initiative is in the process of creating an atomic clock designed for forthcoming space missions. This advanced clock relies on AI-driven algorithms to minimize its size and power prerequisites. : Crew Interactive Mobile Companion (CIMON) CIMON or Crew Interactive Mobile Companion is a unique robot on the International Space Station (ISS) that helps astronauts. Shaped like a head, it can hear and see, and it's powered by AI. Its job includes finding things, keeping track of supplies, recording experiments, taking videos, and snapping pictures. Created by Airbus and the German Aerospace Center, CIMON makes life and work easier for astronauts in space. These activities are just a glimpse of the numerous ongoing activities in AI and ML for space exploration however, there are so many other discoveries and activities in the related field. Potential Applications of AI in Space There is no doubt that AI and ML exhibit an expansive array of use cases expected to shape the future. Here are a few examples that illustrate how the world of space exploration stands to reap benefits from the integration of AI technologies. 🌌Exploration of the solar system: AI-powered spacecraft could be used to explore our solar system more efficiently and safely. These spacecraft could be programmed to autonomously navigate to different destinations, collect data, and avoid hazards by employing machine learning algorithms as well. 🌌Search for extraterrestrial life: Have you ever asked a question yourself “Are we alone in the universe?”What would happen if human beings have got the clue of aliens’ lives on other planets outsides of the solar system? Definitely, it would be even more interesting to analyze their lifestyles and impacts. So, AI could be used to search for extraterrestrial life. AI-powered systems could analyze data from space telescopes and other sensors to identify potential signs of life. 🌌Development of new space technologies: AI could be used to develop new space technologies (such as new propulsion systems and new ways to generate power in space). These technologies could help us to explore space more deeply and to develop new ways to live and work in space. 🌌Health management on space missions: During the space mission, it can be challenging to establish instant communication with Earth-based experts to address health-related issues in real time.AI is expected to play a crucial role to tackle unpredicted circumstances created during the mission, particularly in the case of deep space exploration. In the future, advanced AI could have the capability to process complex datasets instantly with a higher percentage of accuracy and would be able to initiate "self-driving labs" for automated health-related experiments. 🌌Creation of a spacefaring civilization: AI could help us to create a spacefaring civilization. AI-powered systems could help us to build and maintain space stations, mine asteroids, and to travel to other planets. The future of AI in space is full of possibilities. As AI is evolving, we can expect to see even more innovative and groundbreaking applications of this technology in the future. AI could help us to achieve our goals of exploring the universe and becoming a spacefaring civilization. 🌌GPS in Space: has been working on an AI application like GPS in space that would make it easy to explore different planets like  Titan, Mars, and others. So, the lab is an exceptional collaborative platform that brings together researchers, data scientists, and domain experts to tackle some of the most pressing challenges in space exploration using cutting-edge AI and ML techniques. (FDL) NASA Frontier Development Lab 🌌Interstellar Travel and Communication: AI will play a crucial role in interstellar travel where communication delays due to vast distances from Earth. Autonomous AI systems could handle complex decisions without real-time input from Earth by allowing spacecraft to adapt to changing conditions and navigate distant stars while maintaining contact with mission control on a delayed basis. 🌌Swarm Robotics for Celestial Exploration: Swarm robotics (where multiple small robots collaborate to accomplish tasks) could revolutionize celestial exploration. Imagine fleets of small AI-driven rovers roaming across faraway planets, working together to thoroughly study the surroundings. These groups of rovers could quickly map landscapes, run a wide range of experiments, and greatly improve the likelihood of uncovering incredible findings. 🌌Cognitive Assistants for Astronauts: AI-based cognitive assistants could become essential companions for astronauts during long-duration missions. These assistants could provide real-time information, offer solutions to technical problems, and even provide emotional support. By monitoring astronaut health and behaviour, cognitive assistants could alert medical staff to potential issues and help maintain crew well-being. These examples provide just a glimpse of the potential ways AI and ML can be used in the future. There are even more opportunities waiting to be explored. The tested contributions of AI have shown a promising future for space exploration by offering incredible benefits that are hard to imagine now. Challenges and Ethical Considerations While AI has the potential to revolutionize space exploration, there are also some challenges and ethical considerations that need to be addressed. One challenge is that AI systems can be complex and difficult to understand which can make it difficult to ensure that these systems are safe and reliable. Avoiding the potential for AI biases in decision-making, and establishing protocols for AI-aided interstellar communication. Another challenge is that AI systems can be biased which can lead to discrimination against certain groups of people or objects. It is also important to consider the ethical implications of using AI in space. For example, should we use AI to develop autonomous weapons systems? These are just some of the challenges and ethical considerations that need to be addressed as we continue to develop and use AI in space. It is important to have a thoughtful and open discussion about these issues so that we can ensure that AI is used for good and not for harm. Conclusion The integration of AI technologies into space exploration has already transformed how we explore and understand the universe. As we dive deeper into space, AI will undoubtedly become a crucial tool by; enhancing the capabilities of spacecraft, enabling autonomous decision-making, and revolutionizing our approach to celestial exploration. The implementation of AI into modern space exploration has redefined our ability to uncover celestial mysteries from AI-equipped Mars rovers advancing our understanding of distant planets to AI-assisted analysis of cosmic phenomena like gravitational waves and Black Holes. As we look to the future, AI holds promise in autonomous navigation, resource management, data analysis, exoplanet discovery, risk assessment, and more. Initiatives like NASA's AI Exploration Initiative and ESA's ARTES program underscore our commitment to leveraging AI's potential in space. However, challenges surrounding AI reliability, interpretability, bias, and ethical implications must be addressed collaboratively to ensure AI enhances our cosmic exploration responsibly and ethically. The future of AI in space holds the promise of new discoveries, improved efficiency, and a deeper connection to the cosmos. The journey has just begun, and the possibilities are limitless.

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