DOI:
10.18727/0722-6691/5298
ADS BibCode:
2023Msngr.190....3M
Section:
Astronomical Science
Author(s)/Affiliation(s):
Mainieri, V.; Leibundgut, B.; de Jong, R.S.; Mas-Hesse, J.M.; Liske, J.; Lind, K.; Loveday, J.
AA(ESO) AB(ESO) AC(Leibniz Institute for Astrophysics, Potsdam, Germany) AD(Department of Astrophysics, Centre for Astrobiology (CSIC–INTA), Torrejón de Ardoz, Spain) AE(Hamburg Observatory, University of Hamburg, Germany) AF(Department of Physics and Astronomy, Uppsala University, Sweden) AG(University of Sussex, Brighton, UK)

DOI:
10.18727/0722-6691/5299
ADS BibCode:
2023Msngr.190....4T
Section:
Astronomical Science
Author(s)/Affiliation(s):
Toloza, O.; Rebassa-Mansergas, A.; Raddi, R.; Reindl, N.; Gaensicke, B.; Fusillo, N.G.; Scaringi, S.; Belloni, D.; Breedt, E.; Camisassa, M.; Cunningham, T.; de Martino, D.; Ederoclite, A.; Geier, S.; Green, M.; Inight, K.; Kupfer, T.; Maldonado, J.; Marsh, T.; Pala, A.F.; Parsons, S.; Pelisoli, I.; Ren, J.; Rodriguez-Gil, P.; Sahu, S.; Schmidtobreick, L.; Schreiber, M.; Schwope, A.; Steeghs, D.; Szkody, P.; Toonen, S.; Tremblay, P.-E.; Zorotovic, M.
AA(Federico Santa Maria Technical University, Valparaiso, Chile) AB(Catalunya Polytechnic University, Barcelona, Spain) AC(Catalunya Polytechnic University, Barcelona, Spain) AD(Potsdam University, Germany) AE(University of Warwick, Coventry, UK) AF(ESA) AG(Durham University, UK) AH(Federico Santa Maria Technical University, Valparaiso, Chile) AI(University of Cambridge, UK) AJ(Catalunya Polytechnic University, Barcelona, Spain) AK(University of Warwick, Coventry, UK) AL(INAF–Capodimonte Astronomical Observatory, Naples, Italy) AM(University of Sao Paolo Institute of Astronomy, Brazil) AN(Potsdam University, Germany) AO(Tel Aviv University, Israel) AP(University of Warwick, Coventry, UK) AQ(University of California at Santa Barbara, USA) AR(INAF–Palermo Astronomical Observatory, Italy) AS(University of Warwick, Coventry, UK) AT(ESA) AU(University of Sheffield, UK) AV(University of Warwick, Coventry, UK) AW(National Astronomical Observatories – Chaoyang Beijing, China) AX(Canary Islands Institute of Astrophysics, Tenerife, Spain) AY(University of Warwick, Coventry, UK) AZ(ESO) BA(Federico Santa Maria Technical University, Valparaiso, Chile) BB(Leibniz Institute for Astrophysics, Potsdam, Germany) BC(University of Warwick, Coventry, UK) BD(University of Washington, USA) BE(University of Amsterdam, the Netherlands) BF(University of Warwick, Coventry, UK) BG(University of Valparaíso, Chile)
Abstract:
Binary systems containing one or two white dwarfs are important for studying stellar evolution and interactions under a wide range of astrophysical conditions. Thanks to the Gaia mission we have identified the first statistically significant and unbiased sample of ~ 170 000 white dwarf binary candidates. It comprises both systems that never interacted that are part of common proper motion pairs and systems that evolved through mass transfer episodes resulting in close white dwarf binaries. White dwarf binaries hold the potential to observationally constrain a wide variety of key ingredients that currently limit the validity of theoretical models.
References:
Cantat-Gaudin, T. et al. 2018, A&A, 618, A93; Chornay, N. & Walton, N. A. 2021, A&A, 656, A110; El-Badry, K. & Rix, H.-W. 2018, MNRAS, 480, 4884; El-Badry, K., Rix, H.-W. & Heintz, T. M. 2021, MNRAS, 506, 2269; García-Berro, E., Ritossa, C. & Iben, I. 1997, ApJ, 485, 765; Gentile-Fusillo, N. P. et al. 2021, MNRAS, 508, 3877; González-Santamaría, I. et al. 2021, A&A, 656, A51; Ivanova, N. et al. 2013, A&ARv, 21, 59; Jones, D. & Boffin, H. M. J. 2017, Nature Astronomy, 1, 0117; Parsons, S. G. et al. 2016, MNRAS, 463, 2125; Raddi, R. et al. 2022, A&A, 658, A22; Rebassa-Mansergas, A. et al. 2021, MNRAS, 506, 5201; Soderblom, D. R. 2010, ARA&A, 48, 581

DOI:
10.18727/0722-6691/5300
ADS BibCode:
2023Msngr.190....7S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Sacco, G.G.; Jeffries, R.; Binks, A.; Magrini, L.; Damiani, F.; Wright, N.; Prisinzano, L.; Zari, E.; Schneider, C.; Beccari, G.; Weaver, G.; D’Orazi, V.; Biazzo, K.; Nisini, B.; Antoniucci, S.; Franciosini, E.; Robrade, J.; Stelzer, B.; Alfaro, E.J.; Alves, J.; Bayo, A.; Boffin, H.; Bonito, R.; Bouy, H.; Brown, A.; Corbelli, E.; Degl’Innocenti, S.; Fedele, D.; Gagné, J.; Galli, P.; Großschedl, J.; Jerabkova, T.; Kastner, J.; Kawata, D.; Meingast, S.; Miret-Roig, N.; Moraux, E.; Olivares, J.; Parker, R.J.; Moroni, P.G.P.; Prusti, T.; Randich, S.; Roccatagliata, V.; Spina, L.
AA(INAF–Arcetri Astronomical Observatory, Florence, Italy) AB(Astrophysics Group, Keele University, UK) AC(MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA) AD(INAF–Arcetri Astronomical Observatory, Florence, Italy) AE(INAF–Palermo Astronomical Observatory, Italy) AF(Astrophysics Group, Keele University, UK) AG(INAF–Palermo Astronomical Observatory, Italy) AH(Max Planck Institute for Astronomy, Heidelberg, Germany) AI(Hamburg Observatory, University of Hamburg, Germany) AJ(ESO) AK(Astrophysics Group, Keele University, UK) AL(Department of Physics, Tor Vergata University of Rome, Italy; Department of Physics and Astronomy, University of Padua, Italy) AM(INAF–Rome Astronomical Observatory, Italy) AN(INAF–Rome Astronomical Observatory, Italy) AO(INAF–Rome Astronomical Observatory, Italy) AP(INAF–Arcetri Astronomical Observatory, Florence, Italy) AQ(Hamburg Observatory, University of Hamburg, Germany) AR(Institute for Astronomy & Astrophysics, Eberhard Karls University, Tübingen, Germany) AS(Andalucia Institute of Astrophysics (CSIC), Granada, Spain) AT(Department of Astrophysics, University of Vienna, Austria) AU(ESO; Institute of Physics and Astronomy, Faculty of Science, University of Valparaíso, Chile) AV(ESO) AW(INAF–Palermo Astronomical Observatory, Italy) AX(Bordeaux Astrophysics Laboratory, University of Bordeaux, CNRS, Pessac, France) AY(Leiden Observatory, Leiden University, the Netherlands) AZ(INAF–Arcetri Astronomical Observatory, Florence, Italy) BA(Enrico Fermi Department of Physics, University of Pisa, Italy) BB(INAF–Arcetri Astronomical Observatory, Florence, Italy) BC(Rio Tinto Alcan Planetarium, Space For Life, Montreal, Canada; Institute for Research on Exoplanets, Department of Physics, University of Montreal, Canada) BD(Centre for Theoretical Astrophysics, São Paulo City University, Brazil) BE(Department of Astrophysics, University of Vienna, Austria) BF(ESO) BG(School of Physics and Astronomy, Rochester Institute of Technology, NY, USA) BH(Mullard Space Science Laboratory, University College London, UK) BI(Department of Astrophysics, University of Vienna, Austria) BJ(Department of Astrophysics, University of Vienna, Austria) BK(University of Grenoble Alpes, CNRS, IPAG, France) BL(National University for Distance Learning, Spain) BM(Department of Physics and Astronomy, University of Sheffield, UK) BN(Enrico Fermi Department of Physics, University of Pisa, Italy) BO(European Space Agency, European Space Research and Technology Centre (ESTEC), the Netherlands) BP(INAF–Arcetri Astronomical Observatory, Florence, Italy) BQ(INAF–Arcetri Astronomical Observatory, Florence, Italy) BR(Department of Physics and Astronomy, University of Padua, Italy)
Abstract:
Most nearby young stars (with ages < 100 Myr) in the Galactic disc no longer reside in their dense, clustered birthplaces; they are found all around us. The 4MOST Survey of Young Stars will identify a representative sample of about 10⁵ young, low-mass stars within 500 pc of the Sun and will measure their chemistry, 3D kinematics and ages in order to: trace the spatial and dynamical evolution of star-forming structures; quantify the star formation rate and chemical inhomogeneity in the local disc; vastly expand the number of identified young stars for exoplanetary studies; and provide huge coeval samples to improve young stellar evolutionary models.
References:
Adams, F. C. 2010, ARA&A, 48, 47; Alfaro, E. J. et al. 2022, ApJ, 937, 114; Beccari, G., Boffin H. & Jerabkova, T. 2020, MNRAS, 491, 2205; Cantat-Gaudin, T. 2022, Universe, 8, 111; Gagné, J. & Faherty, J. K. 2018, ApJ, 862, 138; Gagné, J. et al. 2021, ApJL, 915, L29; Gaia Collaboration et al. 2022, arXiv:2208.00211; Kounkel, M. & Covey, K. 2019, AJ, 158, 122; Krumholz, M. R., McKee, C. F. & Bland-Hawthorn, J. 2019, ARA&A, 57, 227; Lada, C. J. & Lada, E. A. 2003, ARA&A, 41, 57; Meingast, S., Alves, J. & Rottensteiner, A. 2021, A&A, 645, A84; Predehl, P. et al. 2021, A&A, 647, A1; Prisinzano L. et al. 2022, A&A, 664, A175; Ricker, G. R. et al. 2015, JATIS, 1, 014003; Riello, M. et al. 2021, A&A, 649, A3; Torres, C. A. O. et al. 2006, A&A, 460, 695; Zari, E. et al. 2018, A&A, 620, A172

DOI:
10.18727/0722-6691/5301
ADS BibCode:
2023Msngr.190...10I
Section:
Astronomical Science
Author(s)/Affiliation(s):
Ibata, R.; Battaglia, G.; Bellazzini, M.; Clementini, G.; Errani, R.; Famaey, B.; Garofalo, A.; Hill, V.; Martin, N.; Mucciarelli, A.; Monari, G.; Posti, L.; Skúladóttir, Á.; Sollima, A.; Siebert, A.; Thomas, G.; Malhan, K.; Freundlich, J.; Arentsen, A.; Yuan, Z.
AA(Strasbourg Astronomical Observatory, CNRS, University of Strasbourg, France) AB(Canary Islands Institute of Astrophysics, Tenerife, Spain) AC(INAF–Bologna Astrophysics and Space Science Observatory, Italy) AD(INAF–Bologna Astrophysics and Space Science Observatory, Italy) AE(Strasbourg Astronomical Observatory, CNRS, University of Strasbourg, France) AF(Strasbourg Astronomical Observatory, CNRS, University of Strasbourg, France) AG(INAF–Bologna Astrophysics and Space Science Observatory, Italy) AH(Lagrange Laboratory, Côte d’Azur Observatory, Côte d’Azur University, Nice, France) AI(Strasbourg Astronomical Observatory, CNRS, University of Strasbourg, France) AJ(INAF–Bologna Astrophysics and Space Science Observatory, Italy) AK(Strasbourg Astronomical Observatory, CNRS, University of Strasbourg, France) AL(Strasbourg Astronomical Observatory, CNRS, University of Strasbourg, France) AM(Department of Physics and Astronomy, University of Florence, Italy) AN(INAF–Bologna Astrophysics and Space Science Observatory, Italy) AO(Strasbourg Astronomical Observatory, CNRS, University of Strasbourg, France) AP(Canary Islands Institute of Astrophysics, Tenerife, Spain) AQ(Max Planck Institute for Astronomy, Heidelberg, Germany) AR(Strasbourg Astronomical Observatory, CNRS, University of Strasbourg, France) AS(Institute of Astronomy, University of Cambridge, UK) AT(Strasbourg Astronomical Observatory, CNRS, University of Strasbourg, France)
Abstract:
The 4GRoundS survey will measure the radial velocities and metallicities of southern RR Lyrae stars in Gaia Data Release 3. These stars have excellent photometric distances, allowing the exquisite Gaia proper motions to be converted into physically useful transverse velocities. Armed with the missing radial velocity, 4GRoundS will provide the community with a dataset that will enable studies of the orbital structure of the halo and outer disc, and allow realistic modelling of these components. It will also enable the identification of coherent dynamically cold streams. Together these analyses will map the mass of the Milky Way out to 100 kpc and test models of the dark sector.
References:
Clementini, G. et al. 2022, arXiv:2206.06278; Deason, A., Belokurov, V. & Evans, N. W. 2011, MNRAS, 416, 2903; Garavito-Camargo, N. et al. 2019, ApJ, 884, 51; Hansen, C. J. et al. 2011, A&A, 527, A65; Ibata, R. et al. 2021, ApJ, 914, 123; Iorio, G. & Belokurov, V. 2021, MNRAS, 502, 5686; Kunder, A. et al. 2020, AJ, 159, 270; Laporte, C. F. P. et al. 2018, MNRAS, 481, 286; Muraveva, T. et al. 2018, MNRAS, 481, 1195; Petersen, M. S. & Peñarrubia, J. 2021, Nature Astronomy, 5, 251; Posti, L. & Helmi, A. 2019, A&A, 621, A56; Savino, A. et al. 2020, A&A, 641, 96; Sesar, B. 2012, AJ, 144, 114; Sesar, B. et al. 2014, ApJ, 793, 135; Stringer, K. M. et al. 2021, ApJ, 911, 109; Thomas, G. F. et al. 2019, ApJ, 886, 10; Wegg, C., Gerhard, O. & Bieth, M. 2019, MNRAS, 485, 3296

DOI:
10.18727/0722-6691/5302
ADS BibCode:
2023Msngr.190...13L
Section:
Astronomical Science
Author(s)/Affiliation(s):
Lucatello, S.; Bragaglia, A.; Vallenari, A.; Cantat-Gaudin, T.; Kuzma, P.; Guarcello, M.G.; Spina, L.; Aguado, D.; Carrera, R.; Castro-Ginard, A.; Damiani, F.; D’Orazi, V.; Prisinzano, L.; Valenti, E.; Alfaro, E.; Balaguer-Nuñez, L.; Balbinot, E.; Barrado, D.; Baumgardt, H.; Bellazzini, M.; Bonito, R.; Bossini, D.; Carraro, G.; Carretta, E.; Catanzaro, G.; Casamiquela, L.; Cassisi, S.; Dalessandro, E.; De Silva, G.M.; Ferguson, A.; Ferraro, F.R.; Frasca, A.; Galli, P.; Gieles, M.; Gran, F.; Gratton, R.; Hilker, M.; Jeffries, R.; Jordi, C.; Korn, A.J.; Lanzoni, B.; Larsen, S.; Lattanzio, J.; Lugaro, M.; Mapelli, M.; Massari, D.; Miglio, A.; Miret-Roig, N.; Momany, Y.; Mucciarelli, A.; Olivares, J.; Pasquato, M.; Roccatagliata, V.; Salaris, M.; Schiavon, R.; Smiljanic, R.; Sollima, A.; Tautvaišienė, G.; Varri, A.L.; Wright, N.
AA(INAF–Padua Astronomical Observatory, Italy; Institute for Advanced Studies, Technical University of Munich, Germany) AB(INAF–Bologna Astrophysics and Space Science Observatory, Italy) AC(INAF–Padua Astronomical Observatory, Italy) AD(Max Planck Institute for Astronomy, Heidelberg, Germany) AE(University of Edinburgh, UK) AF(INAF–Palermo Astronomical Observatory, Italy) AG(Department of Physics and Astronomy, University of Padua, Italy) AH(Canary Islands Institute of Astrophysics, Tenerife, Spain) AI(INAF–Padua Astronomical Observatory, Italy) AJ(Leiden Observatory, Leiden University, the Netherlands) AK(INAF–Palermo Astronomical Observatory, Italy) AL(INAF–Padua Astronomical Observatory, Italy; Tor Vergata University of Rome, Italy) AM(INAF–Palermo Astronomical Observatory, Italy) AN(ESO) AO(Spanish National Research Council, Granada, Spain) AP(Institute of Cosmos Sciences, University of Barcelona, Spain; Department of Quantum Physics and Astronomy, University of Barcelona, Spain; Catalunya Institute of Space Studies, Barcelona, Spain) AQ(Leiden Observatory, Leiden University, the Netherlands; University of Groningen,  the Netherlands) AR(Centre for Astrobiology (CSIC-INTA), Torrejón de Ardoz, Spain) AS(University of Queensland, Australia) AT(INAF–Bologna Astrophysics and Space Science Observatory, Italy) AU(INAF–Palermo Astronomical Observatory, Italy) AV(Institute of Astrophysics and Space Science – Porto and Lisbon, Portugal) AW(Department of Physics and Astronomy, University of Padua, Italy) AX(INAF–Bologna Astrophysics and Space Science Observatory, Italy) AY(INAF–Catania Astronomical Observatory, Italy) AZ(GEPI – Paris Observatory, France) BA(INAF–Abruzzo Astronomical Observatory, Italy) BB(INAF–Bologna Astrophysics and Space Science Observatory, Italy) BC(Macquarie University, Australia) BD(University of Edinburgh, UK) BE(Department of Physics and Astronomy, University of Bologna, Italy; INAF–Bologna Astrophysics and Space Science Observatory, Italy) BF(INAF–Catania Astronomical Observatory, Italy) BG(São Paulo City University, Brazil) BH(Institute of Cosmos Sciences, University of Barcelona, Spain; Catalan Institution for Research and Advanced Studies, Barcelona, Spain) BI(Lagrange Laboratory, Côte d’Azur Observatory, Côte d’Azur University, Nice, France) BJ(INAF–Padua Astronomical Observatory, Italy) BK(ESO) BL(Keele University, UK) BM(Institute of Cosmos Sciences, University of Barcelona, Spain; Department of Quantum Physics and Astronomy, University of Barcelona, Spain; Catalunya Institute of Space Studies, Barcelona, Spain) BN(Uppsala University, Sweden) BO(Department of Physics and Astronomy, University of Bologna, Italy; INAF–Bologna Astrophysics and Space Science Observatory, Italy) BP(Radboud University, Nijmegen, the Netherlands) BQ(Monash University, Australia) BR(Konkoly Observatory, CSFK ELKH, Budapest, Hungary) BS(Department of Physics and Astronomy, University of Padua, Italy; INAF–Padua Astronomical Observatory, Italy) BT(INAF–Bologna Astrophysics and Space Science Observatory, Italy) BU(Department of Physics and Astronomy, University of Bologna, Italy; INAF–Bologna Astrophysics and Space Science Observatory, Italy) BV(University of Vienna, Austria) BW(INAF–Padua Astronomical Observatory, Italy) BX(Department of Physics and Astronomy, University of Bologna, Italy; INAF–Bologna Astrophysics and Space Science Observatory, Italy) BY(National University for Distance Learning, Spain) BZ(Department of Physics and Astronomy, University of Padua, Italy; University of Montreal, Canada) CA(University of Pisa, Italy) CB(Liverpool John Moores University, UK) CC(Liverpool John Moores University, UK) CD(Nicolaus Copernicus Astronomical Center, Warsaw, Poland) CE(INAF–Bologna Astrophysics and Space Science Observatory, Italy) CF(Vilnius University, Lithuania) CG(University of Edinburgh, UK) CH(Keele University, UK)
Abstract:
The 4MOST Stellar Clusters Survey will target essentially all the Galactic globular and open clusters and star-forming regions accessible to 4MOST (about 120 globulars, 1800 open clusters and 80 star-forming regions). This will: shed light on how clusters form, evolve, dissolve, and populate the Milky Way; calibrate complex physics that affects stellar evolution, on which our ability to measure accurate ages ultimately rests; and evaluate the contribution of star clusters to the formation and evolution of the individual Galactic components with unparalleled statistics.
References:
Cantat-Gaudin, T. et al. 2020, A&A, 640, A1; Dias, W. S. et al. 2002, A&A, 389, 871; Gaia Collaboration et al. 2023, A&A, in press, arXiv:2206.05534; Gratton, R. et al. 2019, A&ARev., 27, 8; Massari, D., Koppelman, H. H. & Helmi, A. 2019, A&A, 630, L4; Pfeffer, J. et al. 2018, MNRAS, 475, 4309; Vasiliev, E. & Baumgardt, H. 2021, MNRAS, 505, 5978

DOI:
10.18727/0722-6691/5303
ADS BibCode:
2023Msngr.190...17P
Section:
Astronomical Science
Author(s)/Affiliation(s):
Pawlak, M.; Mazeh, T.; Faigler, S.; Shenar, T.; Sana, H.; Bashi, D.
AA(Astronomical Observatory, Jagiellonian University, Kraków, Poland) AB(School of Physics and Astronomy, Tel Aviv University, Israel) AC(School of Physics and Astronomy, Tel Aviv University, Israel) AD(Anton Pannekoek Institute for Astronomy, Amsterdam, the Netherlands) AE(Institute of Astronomy, KU Leuven, Belgium) AF(School of Physics and Astronomy, Tel Aviv University, Israel)
Abstract:
The goal of the Spectroscopic Discovery of Binaries with Dormant Black Holes survey is to spectroscopically follow up stars that might have dormant compact companions, either black holes or neutron stars. These stars have been identified as ellipsoidal binaries in the Magellanic Clouds by the Optical Gravitational Lensing Experiment (OGLE). A sample of more than 700 ellipsoidals with periods shorter than 10 days will be observed to obtain multi-epoch radial-velocity measurements. 4MOST radial velocities in conjunction with OGLE photometry will allow the determination of the secondary component mass and hence the identification of systems with compact companions.
References:
Breivik, K., Chatterjee, S. & Larson, S. L. 2017, ApJL, 850, L13; Corral-Santana, J. M. et al. 2016, A&A, 587, A61; El-Badry, K. et al. 2023, MNRAS, 518, 1057; Faigler, S. & Mazeh, T. 2011, MNRAS, 415, 3921; Faigler, S. et al. 2012, ApJ, 746, 185; Foellmi, C., Moffat, A. F. J. & Guerrero, M. A. 2003, MNRAS, 338, 1025; Langer, N. et al. 2020, A&A, 638, A39; Mazeh, T. 2008, EAS, 29, 1; Pawlak, M. et al. 2016, AcA, 66, 421; Remillard, R. A. & McClintock, J. E. 2006, ARA&A, 44, 49; Tetarenko, B. E. et al. 2016, ApJS, 222, 15; Shenar, T. et al. 2022, Nature Astronomy, 6, 1085; Schnurr, O. et al. 2008, MNRAS, 389, 806; Udalski, A., Szymański, M. K. & Szymański, G. 2015, AcA, 65, 1

DOI:
10.18727/0722-6691/5304
ADS BibCode:
2023Msngr.190...19S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Skúladóttir, Á.; Puls, A.A.; Amarsi, A.M.; Battaglia, G.; Buder, S.; Campbell, S.; Cardona-Barrero, S.; Christlieb, N.; Feuillet, D.K.; Gelli, V.; Hansen, C.J.; Hill, V.; Ibata, R.; Jablonka, P.; Kacharov, N.; Karakas, A.; Koch-Hansen, A.J.; Lind, K.; Lombardo, L.; Lucchesi, R.E.R.; Lugaro, M.; Martin, N.; Massari, D.; Nordlander, T.; Reichert, M.; Rossi, M.; Ruiter, A.J.; Salvadori, S.; Seitenzahl, I.R.; Tolstoy, E.; Xylakis-Dornbusch, T.; Youakim, K.C.
AA(Department of Physics and Astronomy, University of Florence, Italy; INAF–Arcetri Astronomical Observatory, Florence, Italy) AB(Institute of Applied Physics, Goethe University Frankfurt, Germany) AC(Theoretical Astrophysics, Department of Physics and Astronomy, Uppsala University, Sweden) AD(Canary Islands Institute of Astrophysics, Tenerife, Spain; University of La Laguna, Tenerife, Spain) AE(Research School of Astronomy and Astrophysics, Australian National University, Canberra, Australia; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions, Australia) AF(ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions, Australia; School of Physics and Astronomy, Monash University, Australia) AG(Canary Islands Institute of Astrophysics, Tenerife, Spain; University of La Laguna, Tenerife, Spain) AH(Astronomy Centre, Heidelberg University, Germany.) AI(Department of Astronomy and Theoretical Physics, Lund Observatory, Sweden) AJ(Department of Physics and Astronomy, University of Florence, Italy; INAF–Arcetri Astronomical Observatory, Florence, Italy) AK(Institute of Applied Physics, Goethe University Frankfurt, Germany; Max Planck Institute for Astronomy, Heidelberg, Germany) AL(Lagrange Laboratory, Côte d’Azur Observatory, Côte d’Azur University, Nice, France) AM(Strasbourg Astronomical Observatory, CNRS, University of Strasbourg, France) AN(Astrophysics Laboratory, Physics Institute, École Polytechnique Fédérale, Lausanne, Switzerland) AO(Leibniz Institute for Astrophysics, Potsdam, Germany) AP(ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions, Australia; School of Physics and Astronomy, Monash University, Australia) AQ(Computational Astronomy Institute, Centre for Astronomy, Heidelberg University, Germany) AR(Department of Astronomy, Stockholm University, Sweden) AS(GEPI, Paris Observatory, France) AT(Department of Physics and Astronomy, University of Florence, Italy) AU(Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Eötvös Loránd Research Network, Budapest, Hungary; CSFK, MTA Centre of Excellence, Budapest, Hungary; Institute of Physics, ELTE Eötvös Loránd University, Budapest, Hungary; School of Physics and Astronomy, Monash University, Australia) AV(Strasbourg Astronomical Observatory, CNRS, University of Strasbourg, France; Max Planck Institute for Astronomy, Heidelberg, Germany) AW(INAF–Bologna Astrophysics and Space Science Observatory, Italy) AX(Research School of Astronomy and Astrophysics, Australian National University, Canberra, Australia; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions, Australia) AY(Department of Astronomy and Astrophysics, University of València, Spain) AZ(Department of Physics and Astronomy, University of Florence, Italy; INAF–Arcetri Astronomical Observatory, Florence, Italy) BA(School of Science, University of New South Wales, Sydney, Australia) BB(Department of Physics and Astronomy, University of Florence, Italy; INAF–Arcetri Astronomical Observatory, Florence, Italy) BC(School of Science, University of New South Wales, Sydney, Australia) BD(Kapteyn Astronomical Institute, University of Groningen, the Netherlands) BE(Astronomy Centre, Heidelberg University, Germany.; International Max Planck Research School for Astronomy & Cosmic Physics at the University of Heidelberg, Germany) BF(Department of Astronomy, Stockholm University, Sweden)
Abstract:
The present-day Milky Way is the result of a long history of mergers and interactions with smaller galaxies. The 4DWARFS survey will target the dwarf galaxies and stellar streams in the 4MOST footprint, and unveil their chrono-chemo-kinematical properties. The survey will provide radial velocities, chemical abundances and stellar ages for 140 000 stars, and thus increase the number of stars with detailed information in such systems by several orders of magnitude. 4DWARFS will provide a new, deeper view of the Milky Way environment, shedding light on the first stars, chemical evolution, dark matter halos, and hierarchical galaxy formation down to the smallest scales.
References:
Battaglia, G. et al. 2022, A&A, 657, A54; Cicuendez, L. & Battaglia, G. 2018, MNRAS, 480, 251; Feuillet, D. K. et al 2016, ApJ, 817, 40; Gaia collaboration et al. 2018, A&A, 616, A12; Hansen, C. J. et al. 2020, A&A, 643, A49; Ibata, R. et al. 2021, ApJ, 914, 123; Iwamoto, N. et al. 2005, Science, 309, 451; Maoz, D., Mannucci, F. & Nelemans, G. 2014, ARA&A, 52, 107; Martin, N. F. et al. 2016, ApJ, 818, 40; Massari, D. et al. 2018, Nature Astronomy, 2, 156; Rossi, M., Salvadori, S. & Skúladóttir, Á. 2021, MNRAS, 503, 6026; Skúladóttir, Á. & Salvadori. S. 2020, A&A, 634, L2; Tolstoy, E., Hill, V. & Tosi, M. 2009, ARA&A, 47, 371; Xylakis-Dornbusch, T. et al. 2022, A&A, 666, A58

DOI:
10.18727/0722-6691/5305
ADS BibCode:
2023Msngr.190...22I
Section:
Astronomical Science
Author(s)/Affiliation(s):
Iovino, A.; Mercurio, A.; Gallazzi, A.R.; La Barbera, F.; Longhetti, M.; Tortora, C.; Zibetti, S.; Belfiore, F.; Bianconi, M.; Busarello, G.; Corsini, E.M.; Costantin, L.; De Lucia, G.; De Propris, R.; D’Eugenio, F.; Fontanot, F.; García-Benito, R.; Hirschmann, M.; Haines, C.; Mannucci, F.; McGee, S.; Merluzzi, P.; Morelli, L.; Moretti, A.; Pasquali, A.; Poggianti, B.; Pozzetti, L.; Rodighiero, G.; Sánchez-Blázquez, P.; van der Wel, A.; Vazdekis, A.; Vulcani, B.; Zanella, A.; Annunziatella, M.; Concas, A.; Cassarà, L.P.; Cresci, G.; Curti, M.; de Lorenzo-Cáceres, A.; Mateu, A.F.; Delgado, R.M.G.; Mancini, C.; Pacifici, C.; Perez-Montero, E.; Pizzella, A.; Perez-Gonzalez, P.G.; Trager, S.C.; Vergani, D.
AA(INAF–Brera Astronomical Observatory, Italy) AB(INAF–Capodimonte Astronomical Observatory, Naples, Italy) AC(INAF–Arcetri Astronomical Observatory, Florence, Italy) AD(INAF–Capodimonte Astronomical Observatory, Naples, Italy) AE(INAF–Brera Astronomical Observatory, Italy) AF(INAF–Capodimonte Astronomical Observatory, Naples, Italy) AG(INAF–Arcetri Astronomical Observatory, Florence, Italy) AH(INAF–Arcetri Astronomical Observatory, Florence, Italy) AI(University of Birmingham, UK) AJ(INAF–Capodimonte Astronomical Observatory, Naples, Italy) AK(University of Padua, Italy) AL(Centre for Astrobiology (CSIC-INTA), Torrejón de Ardoz, Spain) AM(INAF–Trieste Astronomical Observatory, Italy) AN(Turku University, Finland) AO(Kavli Institute for Cosmology, Cambridge, UK) AP(INAF–Trieste Astronomical Observatory, Italy) AQ(Andalucia Institute of Astrophysics, Granada, Spain) AR(INAF–Trieste Astronomical Observatory, Italy) AS(University of Atacama, Copiapò, Chile) AT(INAF–Arcetri Astronomical Observatory, Florence, Italy) AU(University of Birmingham, UK) AV(INAF–Capodimonte Astronomical Observatory, Naples, Italy) AW(University of Atacama, Copiapò, Chile) AX(INAF–Padua Astronomical Observatory, Italy) AY(Heidelberg University, Germany) AZ(INAF–Padua Astronomical Observatory, Italy) BA(INAF–Bologna Astrophysics and Space Science Observatory, Italy) BB(University of Padua, Italy) BC(Madrid Complutense University, Spain) BD(Ghent University, Belgium) BE(Canary Islands Institute of Astrophysics, Tenerife, Spain) BF(INAF–Padua Astronomical Observatory, Italy) BG(INAF–Padua Astronomical Observatory, Italy) BH(Centre for Astrobiology (CSIC-INTA), Torrejón de Ardoz, Spain) BI(ESO) BJ(INAF–Institute of Space Astrophysics and Cosmic Physics, Milan, Italy) BK(INAF–Arcetri Astronomical Observatory, Florence, Italy) BL(Kavli Institute for Cosmology, Cambridge, UK) BM(Canary Islands Institute of Astrophysics, Tenerife, Spain) BN(Canary Islands Institute of Astrophysics, Tenerife, Spain) BO(Andalucia Institute of Astrophysics, Granada, Spain) BP(University of Padua, Italy) BQ(Space Telescope Science Institute, Baltimore, USA) BR(Andalucia Institute of Astrophysics, Granada, Spain) BS(University of Padua, Italy) BT(Centre for Astrobiology (CSIC-INTA), Torrejón de Ardoz, Spain) BU(University of Groningen, the Netherlands) BV(INAF–Bologna Astrophysics and Space Science Observatory, Italy)
Abstract:
Galaxy spectra encode in their continuum and absorption/emission features a wealth of information on galaxy physics, mass assembly and chemical enrichment history. The 4MOST-StePS survey will collect high-quality spectra (with a median signal-to-noise ratio of about 30 Å^–1, and resolution R ~ 5000) for a sample of about 3300 galaxies brighter than I_AB = 20.5 within the RA-Dec-z footprint of the WAVES-Deep survey. These spectra will provide a precise empirical description of the evolutionary path of massive galaxies in the intermediate redshift range (0.3 < z < 0.7) between the LEGA-C and SDSS surveys. The locations of the galaxies within the cosmic web, unveiled by WAVES-Deep, will disclose the connection between galaxy properties and environment, down to the scales of galaxy pairs.
References:
Bruzual, G. & Charlot, S. 2003, MNRAS, 344, 1000; Carretero, C. et al. 2004, ApJ, 609, L45; Chabrier, G. 2003, PASP, 115, 763; Chauke, P. et al. 2018, ApJ, 861, 13; Concas, A. et al. 2017, MNRAS, 468, 1747; Concas, A. et al. 2019, A&A, 622, A188; Driver, S. P. et al. 2019, The Messenger, 175, 46; Fontanot, F. et al. 2017, MNRAS, 464, 3812; Fontanot, F. et al. 2021, MNRAS, 504, 4481; Gallazzi, A. et al. 2005, MNRAS, 362, 41; Gallazzi, A. et al. 2014, ApJ, 788, 72; Hirschmann, M. et al. 2017, MNRAS, 472, 2468; Hunt, L. et al. 2020, A&A, 643, A180; Iovino, A. et al. 2022, submitted to A&A Maiolino, R. & Mannucci, F. 2019, A&ARv, 27, 3; Sánchez-Blázquez, P. et al. 2003, ApJ, 590, L91; Speagle, J. S. et al. 2014, ApJS, 214, 15; Tortora, C., Romanowsky, A. J. & Napolitano, N. R. 2013, ApJ, 765, 8; Tortora, C. et al. 2018, MNRAS, 473, 969; van der Wel, A. et al. 2021, ApJS, 256, 44; Wu, P.-F. et al. 2021, AJ, 162, 201; York, D. G. et al. 2000, AJ, 120, 1579

DOI:
10.18727/0722-6691/5306
ADS BibCode:
2023Msngr.190...25D
Section:
Astronomical Science
Author(s)/Affiliation(s):
Duncan, K.; Baker, A.; Best, P.; Blyth, S.; Hatch, N.; Holwerda, B.; Jarvis, M.; Maddox, N.; Smith, D.J.B.; Arnaudova, M.; Chemin, L.; Davé, R.; Dunlop, J.; Frank, B.; Gawiser, E.; Gloudemans, A.; Hale, C.; Heywood, I.; Kannappan, S.; Kondapally, R.; McLure, R.; Morabito, L.; Nesvadba, N.; Pan, H.; Ponomareva, A.; Prescott, M.; Roberts, H.; Röttgering, H.; Somerville, R.; Tudorache, M.; Vaccari, M.; Whittam, I.; Wu, J.; Zwaan, M.
AA(University of Edinburgh, UK) AB(Rutgers University, USA) AC(University of Edinburgh, UK) AD(University of Cape Town, South Africa) AE(University of Nottingham, UK) AF(University of Louisville, USA) AG(University of Oxford, UK) AH(University of Bristol, UK) AI(University of Hertfordshire, UK) AJ(University of Hertfordshire, UK) AK(Andres Bello University, Santiago, Chile) AL(University of Edinburgh, UK) AM(University of Edinburgh, UK) AN(South African Radio Astronomy Observatory, South Africa) AO(Rutgers University, USA) AP(Leiden University, the Netherlands) AQ(University of Edinburgh, UK) AR(University of Oxford, UK) AS(University of North Carolina at Chapel Hill, USA) AT(University of Edinburgh, UK) AU(University of Edinburgh, UK) AV(Durham University, UK) AW(Lagrange Laboratory, Côte d’Azur Observatory, Côte d’Azur University, Nice, France) AX(South African Radio Astronomy Observatory, South Africa) AY(University of Oxford, UK) AZ(University of the Western Cape, South Africa) BA(University of Colorado at Boulder, USA) BB(Leiden University, the Netherlands) BC(Flatiron Institute, New York, USA) BD(University of Oxford, UK) BE(University of Cape Town, South Africa) BF(University of Oxford, UK) BG(Space Telescope Science Institute, USA) BH(ESO)
Abstract:
Galaxy evolution is regulated by the continuous cycle of gas accretion, consumption and feedback. Crucial in this cycle is the availability of neutral atomic (HI) and molecular hydrogen. Our current inventory of HI, however, is very limited beyond the local Universe (z > 0.25), resulting in an incomplete picture. ORCHIDSS is designed to address this critical challenge, using the powerful combination of 4MOST spectroscopy and sensitive radio observations from the MeerKAT deep extragalactic surveys to trace the evolution of neutral gas and its lifecycle within galaxies across the bulk of cosmic history.
References:
Bigiel, F. et al. 2011, ApJL, 730, L13; Blyth, S. et al. 2016, Proc. of Science, 277 (MeerKAT2016), 4; Catinella, B. & Cortese, L. 2015, MNRAS, 446, 3526; Catinella, B. et al. 2018, MNRAS, 476, 875; Chowdhury, A., Kanekar, N. & Chengalur, J. N. 2022, ApJ, 937, 103; Davé, R. et al. 2020, MNRAS, 497, 146; Driver, S. P. et al. 2019, The Messenger, 175, 46; Glowacki, M. et al. 2022, ApJL, 931, L7; Heywood, I. et al. 2022, MNRAS, 509, 2150; Kereš, D. et al. 2005, MNRAS, 363, 2; McGaugh, S. S. et al. 2000, ApJL, 533, L99; Pan, H. et al. 2020, MNRAS, 491, 1227; Somerville, R. S. & Davé, R. 2015, ARA&A, 53, 51

DOI:
10.18727/0722-6691/5307
ADS BibCode:
2023Msngr.190...28G
Section:
Astronomical Science
Author(s)/Affiliation(s):
Gruen, D.; McCullough, J.; Amon, A.; Bernstein, G.; van den Busch, J.L.; Canning, R.; Castander, F.; DeRose, J.; Hartley, W.; Hildebrandt, H.; Kuijken, K.; Liske, J.; Masters, D.; Miquel, R.; Yuste, A.P.; Roodman, A.; Seitz, S.; Saglia, R.; Stern, D.; Tortorelli, L.; Wright, A.H.
AA(University Observatory, Faculty of Physics, Ludwig Maximilians University, Munich, Germany) AB(Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, USA; SLAC National Accelerator Laboratory, USA; University Observatory, Faculty of Physics, Ludwig Maximilians University, Munich, Germany) AC(Institute of Astronomy, University of Cambridge, UK; Kavli Institute for Cosmology, University of Cambridge, UK) AD(Department of Physics & Astronomy, University of Pennsylvania, USA) AE(German Centre for Cosmological Lensing, Astronomical Institute, Faculty of Physics and Astronomy, Ruhr University Bochum, Germany) AF(Institute of Cosmology and Gravitation, University of Portsmouth, UK) AG(Catalunya Institute of Space Studies, Barcelona, Spain; Institute of Space Sciences (ICE, CSIC), Barcelona, Spain) AH(Lawrence Berkeley National Laboratory, Berkeley, USA) AI(Department of Astronomy, University of Geneva, Switzerland) AJ(German Centre for Cosmological Lensing, Astronomical Institute, Faculty of Physics and Astronomy, Ruhr University Bochum, Germany) AK(Leiden Observatory, Leiden University, the Netherlands) AL(Hamburg Observatory, University of Hamburg, Germany) AM(IPAC, California Institute of Technology, USA) AN(Institute of High-Energy Physics, Barcelona Institute of Science of Technology, Spain; Catalan Institution for Research and Advanced Studies, Barcelona, Spain) AO(Catalunya Institute of Space Studies, Barcelona, Spain; Institute of Space Sciences (ICE, CSIC), Barcelona, Spain) AP(Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, USA; SLAC National Accelerator Laboratory, USA) AQ(University Observatory, Faculty of Physics, Ludwig Maximilians University, Munich, Germany) AR(University Observatory, Faculty of Physics, Ludwig Maximilians University, Munich, Germany) AS(Jet Propulsion Laboratory, California Institute of Technology, USA) AT(University Observatory, Faculty of Physics, Ludwig Maximilians University, Munich, Germany) AU(German Centre for Cosmological Lensing, Astronomical Institute, Faculty of Physics and Astronomy, Ruhr University Bochum, Germany)
Abstract:
Accurate knowledge of the redshift distributions of faint samples of galaxies selected by broad-band photometry is a prerequisite for future weak lensing experiments to deliver precision tests of our cosmological model. The most direct way to measure these redshift distributions is spectroscopic follow-up of representative galaxies. For this to be efficient and accurate, targets have to be selected such that they systematically cover a space defined by apparent colours in which there is little variation in redshift at any point. 4C3R2 will follow this strategy to observe over 100 000 galaxies selected by their KiDS-VIKING ugriZYJHKs photometry over a footprint identical to that of the WAVES survey, to constrain the colour-redshift relation with high multiplicity across two-thirds of the colour space of future Euclid and Rubin samples.
References:
Buchs, R. et al. 2019, MNRAS, 489, 820; Driver, S. P. et al. 2019, The Messenger, 175, 46; Euclid Collaboration et al. 2020, A&A, 642, A192; Gruen, D. & Brimioulle, F. 2017, MNRAS, 468, 1, 769; Hildebrandt, H. et al. 2017, MNRAS, 465, 1454; Hildebrandt, H. et al. 2021, A&A, 647, A124; Masters, D. et al. 2015, ApJ, 813, 53; Masters, D. C. et al. 2017, ApJ, 841, 111; Masters, D. C. et al. 2019, ApJ, 877, 81; Myles, J. et al. 2021, MNRAS, 505, 4249; Newman, J. A. & Gruen, D. 2022, ARAA, 60, 363; Rau, M. M. et al. 2022, arXiv:2211.16516

DOI:
10.18727/0722-6691/5308
ADS BibCode:
2023Msngr.190...31H
Section:
Astronomical Science
Author(s)/Affiliation(s):
Haines, C.; Jaffé, Y.; Tejos, N.; Monachesi, A.; Pompei, E.; Finoguenov, A.; Sifón, C.; Lopez, S.; Manjunatha, A.B.; Bilton, L.; Comparat, J.; Cuellar, R.; D’Ago, G.; Demarco, R.; Lima-Dias, C.; Lösch, E.; Merluzzi, P.; Castelli, A.S.; Sodre, L.; Vinicius, E.; and the CHANCES team
AA(University of Atacama, Copiapó, Chile) AB(University of Valparaíso, Chile) AC(Pontificia Universidad Católica de Valparaíso) AD(University of La Serena, Chile) AE(ESO) AF(University of Helsinki, Finland) AG(Pontificia Universidad Católica de Valparaíso) AH(University of Chile, Santiago, Chile) AI(University of Atacama, Copiapó, Chile) AJ(University of Valparaíso, Chile; Pontificia Universidad Católica de Valparaíso) AK(Max Planck Institute for Extraterrestrial Physics, Germany) AL(University of Chile, Santiago, Chile) AM(Pontificia Universidad Católica de Chile) AN(University of Concepción, Chile) AO(University of La Serena, Chile) AP(University of São Paulo, Brazil) AQ(INAF–Capodimonte Astronomical Observatory, Naples, Italy) AR(La Plata Institute of Astrophysics (CONICET–UNLP), Argentina; National University of La Plata, Argentina) AS(University of São Paulo, Brazil) AT(University of São Paulo, Brazil)
Abstract:
CHANCES, the CHileAN Cluster galaxy Evolution Survey, will study the evolution of galaxies in and around ~ 150 massive galaxy clusters, from the local Universe out to z ~ 0.45. It will target ~ 300 000 r_AB < 20.5 galaxies with 4MOST, providing comprehensive spectroscopic coverage of each cluster out to 5r₂₀₀ in synergy with eROSITA. Its wide and deep scope will trace massive and dwarf galaxies from the surrounding filaments and groups to the cores of galaxy clusters, enabling the study of galaxy pre-processing and the role of the evolving environment on galaxies. We will also study the effect of clusters on the cold circumgalactic medium by targeting 50 000 cluster–QSO pairs.
References:
Arnaud, M. et al. 2021, A&A, 650, A104; Bahé, Y. M. et al. 2013, MNRAS, 430, 3017; Bianconi, M. et al. 2018, MNRAS, 473, L79; Binggeli, B., Sandage, A. & Tammann, G. A. 1988, ARA&A, 26, 509; Boselli A. & Gavazzi G. 2006, PASP, 118, 517; Butcher H. & Oemler A. 1984, ApJ, 285, 426; Choque-Challapa, N. et al. 2021, MNRAS, 507, 6045; Cortese, L., Catinella, B. & Smith, R. 2021, PASA, 38, 35; Dutta, A., Sharma, P. & Nelson, D. 2022, MNRAS, 510, 3561; Eigenthaler, P. et al. 2018, ApJ, 855, 142; Finoguenov, A. et al. 2020, A&A, 638, A114; Haines, C. P. et al. 2009, ApJ, 704, 126; Haines, C. P. et al. 2015, ApJ, 806, 101; Kuchner, U. et al. 2020, MNRAS, 494, 5473; Lima, E. V. R. et al. 2022, A&C, 38, 100510; Lopez, S. et al. 2008, ApJ, 679, 1144; McGee, S. L. et al. 2009, MNRAS, 400, 937; Mendes de Oliveira, C. et al. 2019, MNRAS, 489, 241; Planck Collaboration et al. 2016, A&A, 594, A27; Reiprich, T. H. et al. 2021, A&A, 647, A2; Zabludoff, A. I. et al. 1996, ApJ, 466, 104

DOI:
10.18727/0722-6691/5309
ADS BibCode:
2023Msngr.190...34B
Section:
Astronomical Science
Author(s)/Affiliation(s):
Bauer, F.E.; Lira, P.; Anguita, T.; Arevalo, P.; Assef, R.; Barrientos, F.; Berg, T.; Bernal, S.; Bian, F.; Boquien, M.; Buat, V.; Chilingarian, I.; Coppi, P.; De Cicco, D.; Diaz, Y.; Grishin, K.; Hernandez-Garcia, L.; Kakkad, D.; Katkov, I.; Krogager, J.-K.; López-Navas, E.; Martínez-Ramírez, L.N.; Mazzucchelli, C.; Motta, V.; Ricci, F.; Ricci, C.; Rojas, A.; Rouse, B.; Sánchez-Sáez, P.; Toptun, V.; Treister, E.; Vito, F.
AA(Pontificia Universidad Católica de Chile, Santiago, Chile; Millennium Institute of Astrophysics, Pontificia Universidad Católica de Chile, Santiago, Chile) AB(University of Chile, Santiago, Chile) AC(Universidad Andrés Bello, Santiago, Chile; Millennium Institute of Astrophysics, Pontificia Universidad Católica de Chile, Santiago, Chile) AD(Universidad de Valparaíso, Chile) AE(Diego Portales University, Santiago, Chile) AF(Pontificia Universidad Católica de Chile, Santiago, Chile) AG(Milan-Bicocca University, Italy) AH(Universidad de Valparaíso, Chile) AI(ESO) AJ(University of Antofagasta, Chile) AK(Marseille Astrophysics Laboratory, France) AL(Center for Astrophysics, Harvard and Smithsonian, USA; Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University, Russia) AM(Yale University, New Haven, USA) AN(Federico II University of Naples, Italy) AO(Diego Portales University, Santiago, Chile) AP(APC Laboratory, University of Paris, France; Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University, Russia) AQ(Millennium Institute of Astrophysics, Pontificia Universidad Católica de Chile, Santiago, Chile; Universidad de Valparaíso, Chile) AR(Space Telescope Science Institute, Baltimore, USA) AS(New York University Abu Dhabi, UAE; Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University, Russia) AT(Lyon Astrophysics Research Centre, France) AU(Universidad de Valparaíso, Chile) AV(Pontificia Universidad Católica de Chile, Santiago, Chile; Millennium Institute of Astrophysics, Pontificia Universidad Católica de Chile, Santiago, Chile) AW(Diego Portales University, Santiago, Chile) AX(Universidad de Valparaíso, Chile) AY(Roma Tre University, Italy) AZ(Diego Portales University, Santiago, Chile) BA(University of Antofagasta, Chile; Diego Portales University, Santiago, Chile) BB(Pontificia Universidad Católica de Chile, Santiago, Chile) BC(ESO) BD(Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University, Russia) BE(Pontificia Universidad Católica de Chile, Santiago, Chile) BF(INAF-OAS, Bologna, Italy)
Abstract:
4MOST-ChANGES will target a legacy sample of active galactic nuclei (AGN), based on optical continuum variability and spectral energy distribution (SED) selection from several existing sur- veys, and ultimately complemented by Rubin LSST to: 1) constrain the low-M_BH, low-L/L_Edd end of the accretion and black hole (BH) density functions to z ~ 1, and, by extension, BH seed models; 2) investigate correlations among AGN (M_BH, L/L_Edd, ultraviolet slope, outflows, variability) and host properties (stellar age, metallicity, kinematics); 3) confirm/characterise rare BH subsamples (extreme variability, tidal disruption events, lensed, intervening absorption line systems) for detailed multi-wavelength follow-up studies.
References:
Aird, J. et al. 2015, MNRAS, 451, 1892; Assef, R. J. et al. 2010, ApJ, 713, 970; Boquien, M. et al. 2019, A&A, 622, 103; De Cicco, D. et al. 2021, A&A, 645, A103; Flesch, E. W. 2021, arXiv:2105.12985; Gezari, S. 2021, ARA&A, 59, 21; Graham, M. J. et al. 2020, MNRAS, 491, 4925; Greene, J. E., Strader, J. & Ho, L. C. 2020, ARA&A, 58, 257; Krogager, J.-K. et al. 2019, MNRAS, 486, 4377; López-Navas, E. et al. 2023, MNRAS, 518, 1531; Luo, Y., Shen, Y. & Yang, Q. 2020, MNRAS, 494, 3686; McGreer, I. D. et al. 2018, AJ, 155, 131; Pâris, I. et al. 2018, A&A, 613, A51; Peters, C. M. et al. 2015, ApJ, 811, 95; Sánchez-Sáez, P. et al. 2019, ApJS, 242, 10; Sánchez-Sáez, P. et al. 2021, AJ, 161, 141; Tie, S. S. et al. 2017, AJ, 153, 107; Volonteri, M. et al. 2017, ApJ, 849, 155

DOI:
10.18727/0722-6691/5310
ADS BibCode:
2023Msngr.190...38K
Section:
Astronomical Science
Author(s)/Affiliation(s):
Krogager, J.-K.; Leighly, K.M.; Fynbo, J.P.U.; Heintz, K.E.; Balashev, S.; Bauer, F.E.; Berg, T.; Choi, H.; Christensen, L.B.; De Cia, A.; Ellison, S.; Geier, S.; Glikman, E.; Gupta, N.; Konstantopoulou, C.; Kosenko, D.; Ledoux, C.; López, S.; Milvang-Jensen, B.; Morabito, L.; Møller, P.; Noterdaeme, P.; Pettini, M.; Prochaska, J.X.; Raimundo, S.; Richard, J.; Srianand, R.; Telikova, K.; Terndrup, D.; Tripp, T.M.; Vestergaard, M.; Zafar, T.
AA(CRAL, University Claude Bernard Lyon 1, ENS of Lyon, France) AB(Homer L. Dodge Department of Physics and Astronomy, The University of Oklahoma, USA) AC(The Cosmic DAWN Center, Denmark; Niels Bohr Institute, University of Copenhagen, Denmark) AD(The Cosmic DAWN Center, Denmark; Niels Bohr Institute, University of Copenhagen, Denmark) AE(Ioffe Institute, Saint Petersburg, Russia) AF(Institute of Astrophysics and Centre for Astroengineering, Faculty of Physics, Pontifical Catholic University of Chile, Santiago, Chile; Millennium Institute of Astrophysics, Santiago, Chile) AG(Ioffe Institute, Saint Petersburg, Russia; Department of Astronomy, University of Chile, Santiago, Chile) AH(Department of Physics, University of Montreal, Canada) AI(The Cosmic DAWN Center, Denmark; Niels Bohr Institute, University of Copenhagen, Denmark) AJ(Department of Astronomy, University of Geneva, Switzerland; ESO) AK(Department of Physics & Astronomy, University of Victoria, Canada) AL(Gran Telescopio Canarias, La Palma, Spain; Canary Islands Institute of Astrophysics, Tenerife, Spain) AM(Department of Physics, Middlebury College, USA) AN(Inter-University Centre for Astronomy and Astrophysics, Pune, India) AO(Department of Astronomy, University of Geneva, Switzerland) AP(Ioffe Institute, Saint Petersburg, Russia) AQ(ESO) AR(Department of Astronomy, University of Chile, Santiago, Chile) AS(The Cosmic DAWN Center, Denmark; Niels Bohr Institute, University of Copenhagen, Denmark) AT(Centre for Extragalactic Astronomy, Department of Physics, Durham University, UK; Institute for Computational Cosmology, Department of Physics, Durham University, UK) AU(Niels Bohr Institute, University of Copenhagen, Denmark; ESO) AV(Paris Institute of Astrophysics, France; French-Chilean Laboratory for Astronomy, Santiago, Chile) AW(Institute of Astronomy, University of Cambridge, UK) AX(Department of Astronomy & Astrophysics, UCO/Lick Observatory, University of California, USA; Kavli Institute for the Physics and Mathematics of the Universe, Kashiwa, Japan) AY(Niels Bohr Institute, University of Copenhagen, Denmark; Department of Physics and Astronomy, University of California, Los Angeles, USA; Department of Physics & Astronomy, University of Southampton, UK) AZ(CRAL, University Claude Bernard Lyon 1, ENS of Lyon, France) BA(Inter-University Centre for Astronomy and Astrophysics, Pune, India) BB(ESO; Ioffe Institute, Saint Petersburg, Russia) BC(Department of Astronomy, The Ohio State University, USA) BD(Department of Astronomy, University of Massachusetts, USA) BE(Niels Bohr Institute, University of Copenhagen, Denmark; Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Denmark) BF(Australian Astronomical Optics, Macquarie University, Australia)
Abstract:
The 4MOST–Gaia Purely Astrometric Quasar Survey (4G-PAQS) will carry out the first large-scale, colour-independent quasar survey selected solely on the basis of astrometry from Gaia. Our main objective is to quantify the selection effects of current colour-selected samples. These colour-selected samples bias our view of the neutral gas and its chemical enrichment because of dust obscuration and reddening of optical colours. Moreover, the broad absorption-line outflows observed in quasars are under-represented by optical colour selection. 4G-PAQS will provide the first sample to overcome these challenges and will constrain the physical and chemical properties of gas in galaxies and quasars at cosmic noon.
References:
Allen, J. T. et al. 2011, MNRAS, 410, 860; Balashev, S. A. & Noterdaeme, P. 2018, MNRAS, 478, 7; Bird, S. et al. 2014, MNRAS, 445, 2313; Bruni, G. et al. 2019, A&A, 630, A111; Choi, H. et al. 2020, ApJ, 891, 53; De Cia, A. et al. 2018, A&A, 611, A76; Fabian, A. C. 2012, ARA&A, 50, 455; Feldmann, R. et al. 2022, arXiv:2205.15325; Fynbo, J. P. U. et al. 2013, ApJS, 204, 6; Geier, S. J. et al. 2019, A&A, 625, L9; Glikman, E. et al. 2012, ApJ, 757, 51; Hall, P. B. et al. 2002, ApJS, 141, 267; Hassan, S. et al. 2020, MNRAS, 492, 2835; Heintz, K. E. et al. 2018, A&A, 615, L8; Heintz, K. E. et al. 2020, A&A, 644, A17; Hewett, P. C. & Foltz, C. B. 2003, AJ, 125, 1784; Kim, D. et al. 2015, ApJ, 812, 66; Krogager, J.-K. et al. 2015, ApJS, 217, 5; Krogager, J.-K. et al. 2019, MNRAS, 486, 4377; Leighly, K. M. et al. 2018, ApJ, 866, 7; Morabito, L. K. et al. 2019, A&A, 622, A15; Nickerson, S., Teyssier, R. & Rosdahl, J. 2019, MNRAS, 484, 1238; Noterdaeme, P. et al. 2014, A&A, 566, A24; Pei, Y. C., Fall, S. M. & Bechtold, J. 1991, ApJ, 378, 6; Péroux, C. & Howk, J. C. 2020, ARA&A, 58, 363; Pontzen, A. & Pettini, M. 2009, MNRAS, 393, 557; Prochaska, J. X. et al. 2003, ApJ, 595, L9; Urrutia, T., Lacy, M. & Becker, R. H. 2008, ApJ, 674, 80; White, R. L. et al. 2003, AJ, 126, 706; Wolfe, A. M., Gawiser, E. & Prochaska, J. X. 2005, ARA&A, 43, 861

DOI:
10.18727/0722-6691/5311
ADS BibCode:
2023Msngr.190...42P
Section:
Astronomical Science
Author(s)/Affiliation(s):
Peroux, C.; Merloni, A.; Liske, J.; Salvato, M.; Augustin, R.; Balzer, F.; Cioni, M.-R.; Comparat, J.; Driver, S.; Fresco, A.; Garzilli, A.; Hamanowicz, A.; Klitsch, A.; Kneib, J.-P.; Krogager, J.-K.; Nelson, D.; Richard, J.; Schady, P.; Shen, Y.; Szakacs, R.; Weng, S.; Yang, Q.; and the ByCycle team
AA(ESO; Marseille Astrophysics Laboratory, France) AB(Max Planck Institute for Extraterrestrial Physics, Garching, Germany) AC(University of Hamburg, Germany) AD(Max Planck Institute for Extraterrestrial Physics, Garching, Germany) AE(Space Telescope Science Institute, USA) AF(Max Planck Institute for Extraterrestrial Physics, Garching, Germany) AG(Leibniz Institute for Astrophysics, Potsdam, Germany) AH(Max Planck Institute for Extraterrestrial Physics, Garching, Germany) AI(International Centre for Radio Astronomy Research/University of Western Australia) AJ(Max Planck Institute for Extraterrestrial Physics, Garching, Germany) AK(École Polytechnique Fédérale, Lausanne, Switzerland) AL(Space Telescope Science Institute, USA) AM(Dark Cosmology Center, Denmark) AN(École Polytechnique Fédérale, Lausanne, Switzerland) AO(CRAL, University Claude Bernard Lyon 1, ENS of Lyon, France) AP(University of Heidelberg, Germany) AQ(CRAL, University Claude Bernard Lyon 1, ENS of Lyon, France) AR(University of Bath, UK) AS(University of Illinois Urbana-Champaign, USA) AT(ESO) AU(ESO) AV(Center for Astrophysics Harvard & Smithsonian, USA)
Abstract:
The term baryons refers to the normal matter of the Universe. Surprisingly, only a minority of this normal matter (< 10%) can be probed by observations of starlight from galaxies. The ByCycle project aims to study the remaining majority of the baryons traced by the intergalactic gas. To this end, ByCycle will use the powerful synergy of absorption and emission diagnostics by observing a large sample of background quasars to probe the circumgalactic medium of foreground objects in the same sky regions. The objective of the 2.8-million fibre-hour ByCycle project is ultimately to characterise the physical processes by which gas changes phases and travels into, through, and out of galaxies. Such a study is essential to our understanding of the growth of structure in the Universe.
References:
Anand, A., Nelson, D. & Kauffmann, G. 2021, MNRAS, 504, 65; Augustin, R. et al. 2021, MNRAS, 505, 6195; Bouwens, R. et al. 2020, ApJ, 902, 112; Byrohl, C. et al. 2021, MNRAS, 506, 5129; Chen, Y. et al. 2021, MNRAS, 508, 19; Chisari, N. E. et al. 2018, MNRAS, 480, 3962; Cooke, R. J., Pettini, M. & Steidel, C. C. 2018, ApJ, 855, 102; Driver, S. P. et al. 2019, The Messenger, 175, 46; Foreman, S. et al. 2020, MNRAS, 498, 2887; Finoguenov, A. 2019, The Messenger, 175, 39; Fumagalli, M. 2017, MNRAS, 467, 4802; Hamanowicz, A. et al. 2020, MNRAS, 492, 2347; Kollmeier, J. A. et al. 2014, ApJL, 789, L32; Quiret, S. et al. 2016, MNRAS, 458, 4074; Macquart, J.-P. et al. 2020, Nature, 581, 391; Madau, P. & Dickinson, M. 2014, ARA&A, 52, 415; Merloni, A. et al. 2019, The Messenger, 175, 42; Mitchell, P. D. & Schaye, J. 2022, MNRAS, 511, 2600; Nelson, D. et al. 2020, MNRAS, 489, 2391; Peeples, M. S. et al. 2014, ApJ, 786, 54; Peeples, M. S. et al. 2019, ApJ, 873, 129; Peroux, C. & Howk, J. C. 2020, ARA&A, 58, 363; Pettini, M. 1999, in Chemical Evolution from Zero to High Redshift, ed. Walsh, J. R. & Rosa, M. R. (Berlin: Springer-Verlag), 233; Planck Collaboration et al. 2016, A&A, 594, A13; Rahmati, A. et al. 2013, MNRAS, 430, 2427; Richard, J. 2019, The Messenger, 175, 50; Salvato, M., Ilbert, O. & Hoyle, B. 2019, Nature Astronomy, 3, 212; Semboloni, E. et al. 2011, MNRAS, 417, 2020; Szakacs, R. et al. 2023, submitted to MNRAS Tacconi, L. J., Genzel, R. & Sternberg, A. 2020, ARA&A, 58, 157; Turner, M. L. et al. 2014, MNRAS, 445, 794; Turner, M. L. et al. 2017, MNRAS, 471, 690; van de Voort, F. et al. 2019, MNRAS, 482, L85; Yang, Q. & Shen, Y. 2023, ApJS, 264, 9; Yates, R. M., Peroux, C. & Nelson, D. 2021, MNRAS, 508, 3535; Walter, F. et al. 2020, ApJ, 902, 111; Zavala, J. A. et al. 2021, ApJ, 909,165

DOI:
10.18727/0722-6691/5312
ADS BibCode:
2023Msngr.190...46T
Section:
Astronomical Science
Author(s)/Affiliation(s):
Taylor, E.N.; Cluver, M.; Bell, E.; Brinchmann, J.; Colless, M.; Courtois, H.; Hoekstra, H.; Kannappan, S.; Lagos, C.; Liske, J.; Tempel, E.; Howlett, C.; McGee, S.; Said, K.; Skelton, R.; Gunawardhana, M.; Bellstedt, S.; Hunt, L.; Jarrett, T.; Lidman, C.; Lucey, J.; Alam, S.; Bilicki, M.; de Graaff, A.; Hellwing, W.; Leslie, S.; Loubser, I.; Marchetti, L.; Maseda, M.; Mogotsi, M.; Norberg, P.; Sonnenfeld, A.; Sorce, J.G.; and the 4HS Team
AA(Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Melbourne, Australia) AB(Department of Physics and Astronomy, University of the Western Cape, South Africa) AC(Department of Astronomy, University of Michigan, USA) AD(Institute of Astrophysics and Space Science, University of Porto, Portugal) AE(Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia) AF(Lyon Institute of Physics of the 2 Infinities, University of Lyon, France) AG(Leiden Observatory, Leiden University, the Netherlands) AH(Department of Physics and Astronomy, The University of North Carolina at Chapel Hill, USA) AI(International Centre for Radio Astronomy Research, University of Western Australia, Perth, Australia; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions, Australia; Cosmic Dawn Center, Denmark) AJ(Hamburg Observatory, University of Hamburg, Germany) AK(Tartu Observatory, University of Tartu, Estonia) AL(School of Mathematics and Physics, University of Queensland, Brisbane, Australia) AM(School of Physics and Astronomy, University of Birmingham, UK) AN(School of Mathematics and Physics, University of Queensland, Brisbane, Australia) AO(South African Astronomical Observatory, Cape Town, South Africa) AP(Sydney Institute for Astronomy, School of Physics, University of Sydney, Australia) AQ(International Centre for Radio Astronomy Research, University of Western Australia, Perth, Australia) AR(INAF–Arcetri Astronomical Observatory, Florence, Italy) AS(Department of Astronomy, University of Cape Town, South Africa) AT(Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia) AU(Department of Physics, Durham University, UK) AV(Tata Institute of Fundamental Research, Mumbai, India) AW(Center for Theoretical Physics, Polish Academy of Sciences, Warsaw, Poland) AX(Max Planck Institute for Astronomy, Heidelberg, Germany) AY(Center for Theoretical Physics, Polish Academy of Sciences, Warsaw, Poland) AZ(Leiden Observatory, Leiden University, the Netherlands) BA(Centre for Space Research, North West University, Potchefstroom, South Africa) BB(Department of Astronomy, University of Cape Town, South Africa; INAF–Institute for Radio Astronomy, Bologna, Italy) BC(Department of Astronomy, University of Wisconsin–Madison, USA) BD(South African Astronomical Observatory, Cape Town, South Africa) BE(Department of Physics, Durham University, UK) BF(Department of Astronomy, School of Physics and Astronomy, Shanghai Jiao Tong University, China) BG(University of Lille, CNRS, France; Institute of Space Astrophysics, University of Paris-Saclay, CNRS, Orsay, France; Leibniz Institute for Astrophysics, Potsdam, Germany)
Abstract:
The 4MOST Hemisphere Survey (4HS) will obtain uniform spectroscopy and redshifts for approximately six million galaxies over ~ 2π steradians, and with high and unbiased completeness for z < 0.15. 4HS aims to 1) complete the map of mass and motion in the Local Volume, 2) map the influence of environment on galaxy evolution through overwhelming statistics, and 3) define the local (z < 0.15) galaxy reference sample for the era of LSST, Euclid, and ASKAP/MeerKAT/SKA. The result is a dataset with exceptional and long-lasting legacy value.
References:
Colless, M. et al. 2001, MNRAS, 328, 1039; Davies, L. J. M. et al. 2019, MNRAS, 483, 5444; Driver, S. P. et al. 2022, MNRAS, 513, 439; Driver, S. P. et al. 2019, The Messenger, 175, 46; Hahn, C. et al. 2022, arXiv:2208.08512; Howlett C. et al. 2022, MNRAS, 515, 953; Jarrett T. H. et al. 2000, AJ, 119, 2498; Kourkchi, E. et al. 2022, MNRAS, 511, 6160; Qin, F. et al. 2018, MNRAS, 477, 5150; Melchior, P. et al. 2018, Astronomy & Computing, 24, 129

DOI:
10.18727/0722-6691/5313
ADS BibCode:
2023Msngr.190...49C
Section:
Astronomical Science
Author(s)/Affiliation(s):
Collett, T.E.; Sonnenfeld, A.; Frohmaier, C.; Glazebrook, K.; Sluse, D.; Motta, V.; Verma, A.; Anguita, T.; Koopmans, L.; Tortora, C.; Courbin, F.; Cabanac, R.; Frye, B.; Smith, G.P.; Diego, J.M.; Alteiri, B.; Lopez, S.; Fassnacht, C.; Cooray, A.; Goobar, A.; Ryczanowski, D.; Serjeant, S.; Richard, J.; Treu, T.; Moustakas, L.; Li, R.; Jacobs, C.; Lemon, C.; Marchetti, L.; Hartley, P.; Jullo, E.; Lee, C.-H.; Birrer, S.; Fritz, A.; Nightingale, J.; Napolitano, N.; Plazas, A.A.; Kruk, S.; Spiniello, C.; Grillo, C.; Suyu, S.; Shajib, A.; Vernardos, G.; Dye, S.; Daylan, T.; Newman, J.; Schuldt, S.
AA(University of Portsmouth, UK) AB(Shanghai Jiao Tong University, Shanghai, China) AC(University of Southampton, UK) AD(Swinburne University of Technology, Australia) AE(University of Liège, Belgium) AF(University of Valparaìso, Chile) AG(University of Oxford, UK) AH(Andres Bello University, Santiago, Chile) AI(University of Groningen, the Netherlands) AJ(INAF–Capodimonte Astronomical Observatory, Naples, Italy) AK(École Polytechnique Fédérale, Lausanne, Switzerland) AL(Midi Pyrénées Observatory, Toulouse, France) AM(University of Arizona, USA) AN(University of Birmingham, UK) AO(Cantabria Institute of Physics, Santander, Spain) AP(ESA – European Space Astronomy Centre, Madrid, Spain) AQ(University of Chile, Santiago, Chile) AR(University of California at Davis, USA) AS(University of California at Irvine, USA) AT(Stockholm University, Sweden) AU(University of Birmingham, UK) AV(The Open University, UK) AW(Lyon Astrophysics Research Centre, France) AX(University of California at Los Angeles, USA) AY(Jet Propulsion Laboratory, Pasadena, USA) AZ(University of Chinese Academy of Sciences & National Astronomical Observatories, PR China) BA(Swinburne University of Technology, Australia) BB(École Polytechnique Fédérale, Lausanne, Switzerland) BC(University of Cape Town, South Africa) BD(Square Kilometre Array Observatory, UK) BE(Marseille Astrophysics Laboratory, France) BF(NSF’s NOIRLab, USA) BG(Stony Brook University, USA) BH(Max Planck Institute for Extraterrestrial Physics, Garching, Germany) BI(Durham University, UK) BJ(INAF–Capodimonte Astronomical Observatory, Naples, Italy) BK(Princeton University, USA) BL(ESA – European Space Research and Technology Centre, Noordwijk, the Netherlands) BM(University of Oxford, UK) BN(University of Milan, Italy) BO(Max Planck Institute for Astrophysics, Garching, Germany) BP(University of Chicago, USA) BQ(École Polytechnique Fédérale, Lausanne, Switzerland) BR(University of Nottingham, UK) BS(Washington University in St. Louis, USA) BT(University of Pittsburgh, USA) BU(University of Milan, Italy)
Abstract:
Almost all science that can be done with strong gravitational lenses requires knowledge of the lens and source redshifts. The 4MOST Strong Lensing Spectroscopic Legacy Survey (4SLSLS) will follow up strong lens candidates discovered in the Euclid survey and the Legacy Survey of Space and Time. 4SLSLS will provide pairs of redshifts for 10 000 strong-lensing galaxies (lenses) and background galaxies (sources). Velocity dispersions will also be measured for 5000 lenses. This sample will enable discoveries about the evolution of galaxies, the study of intrinsically faint objects and of the cosmological model.
References:
Auger, M. W. et al. 2010, ApJ, 724, 511; Barone-Nugent, R. L. et al. 2014, ApJ, 793, 17; Bolton, A. S. et al. 2006, ApJ, 638, 703; Collett, T. E. et al. 2012, MNRAS, 424, 2864; Collett, T. E. 2015, ApJ, 811, 20; Collett, T. E. & Auger, M. W. 2014, MNRAS, 443, 969; Collett, T. E. et al. 2018, Sci, 360, 1342; Dye, S. et al. 2022, MNRAS, 510, 3734; Elbert, O. D. et al. 2018, ApJ, 853, 109; Frye, B., Broadhurst, T. & Benítez, N. 2002, ApJ, 568, 558; Frye, B. et al. 2012, ApJ, 754, 17; Gavazzi, R. et al. 2012, ApJ, 761, 170; Gnedin, O. Y. et al. 2011, arXiv:1108.5736; Grillo, C. et al. 2018, ApJ, 860, 94; Hartley, P. et al. 2017, MNRAS, 471, 3378; Ivezic, Z. et al. 2008, SerAJ, 176, 1; Jacobs, C. et al. 2019, ApJS, 243, 17; Jones, T. et al. 2015, AJ, 149, 107; Jones, T., Stark, D. P. & Ellis, R. S. 2018, ApJ, 863, 191; Laureijs, R. et al. 2011, arXiv:1110.3193; Li, R. et al. 2020, ApJ, 899, 30; Livermore, R. C. et al. 2015, MNRAS, 450, 1812; Marshall, P., Blandford, R. & Sako, M. 2005, NewAR, 49, 387; Martizzi, D., Teyssier, R. & Moore, B. 2013, MNRAS, 432, 1947; Miyazaki, S. et al. 2006, SPIE, 6269, 62690B More, A. et al. 2016, MNRAS, 455, 1191; Myers, S. T. et al. 2003, MNRAS, 341, 1; Napolitano, N. R. et al. 2020, ApJL, 904, L31; Negrello, M. et al. 2014, MNRAS, 440 1999; Newton, E. R. et al. 2011, ApJ, 734, 104; Oldham, L. J. & Auger, M. W. 2018, MNRAS, 476, 133; Peirani, S. et al. 2017, MNRAS, 472, 2153; Petrillo, C. E. et al. 2019, MNRAS, 484, 3879; Pettini, M. et al. 2002, Ap&SS, 281, 461; Rigby, J. R. et al. 2017, ApJ, 843, 79; Ritondale, E. et al. 2019, MNRAS, 485, 2179; Romano-Díaz, E. et al. 2008, ApJL, 685, L105; Schaller, M. et al. 2015, MNRAS, 451, 1247; Schwab, J., Bolton, A. S. & Rappaport, S. A. 2010, ApJ, 708, 750; Shajib, A. J. et al. 2021, MNRAS, 503, 2380; Sonnenfeld, A. & Cautun, M. 2021, A&A, 651, A18; Sonnenfeld, A. et al. 2018, MNRAS, 481, 164; Swinbank, A. M. et al. 2015, ApJL, 806, L17; Vegetti, S. et al. 2014, MNRAS, 442, 2017; Wang, X. et al. 2017, ApJ, 837, 89; Wong, K. C. et al. 2020, MNRAS, 498, 1420; Wuyts, E. et al. 2014, ApJ, 781, 61; Xu, D. et al. 2017, MNRAS, 469, 1824; Yuan, F., Bu, D. & Wu, M. 2012, ApJ, 761, 130; Yuan, T.-T. et al. 2011, ApJL, 732, L14

DOI:
10.18727/0722-6691/5314
ADS BibCode:
2023Msngr.190...55M
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Martinez, P.; Beaulieu, M.; Gouvret, C.; Spang, A.; Marcotto, A.
AA(Lagrange Laboratory, Côte d’Azur Observatory, Côte d’Azur University, CNRS, Nice, France) AB(Lagrange Laboratory, Côte d’Azur Observatory, Côte d’Azur University, CNRS, Nice, France) AC(Lagrange Laboratory, Côte d’Azur Observatory, Côte d’Azur University, CNRS, Nice, France) AD(Lagrange Laboratory, Côte d’Azur Observatory, Côte d’Azur University, CNRS, Nice, France) AE(Lagrange Laboratory, Côte d’Azur Observatory, Côte d’Azur University, CNRS, Nice, France)
Abstract:
The Segmented Pupil Experiment for Exoplanet Detection (SPEED) optical test bed is now ready for operation. SPEED is dedicated to high-contrast imaging at short angular separations with segmented telescopes. Its optical design allows a wide range of applications and the immediate goal is to demonstrate a high-contrast dark hole close to the stellar vicinity. This will be achieved by a combination of optimal wavefront shaping architecture, small inner working angle coronagraphy, and efficient complex field sensor for fine cophasing and dark hole generation.
References:
Beaulieu, M. et al. 2017, MNRAS, 469, 218; Beaulieu, M. et al. 2020, MNRAS, 498, 3914; Blind, N. et al. 2022, Proc. SPIE, 12185, 1218573; Boccaletti, A. et al. 2020, arXiv:2003.05714; Codona, J. L. et al. 2013, Opt. Eng., 52, 097105; Guyon, O. et al. 2014, ApJ, 780, 171; Janin-Potiron, P. et al. 2016, A&A, 592, A110; Kasper, M. et al. 2021, The Messenger, 182, 38; Krist, J. E. et al. 2007, Proc. SPIE, 6675, 66750P Lozi, J. et al. 2018, Proc. SPIE, 10703, 1070359; Males, J. R. et al. 2018, Proc. SPIE, 10703, 1070309; Martinez, P. 2019, A&A, 629, L10; Martinez, P. et al. 2022a, Proc. SPIE, 12184, 121843W Martinez, P. et al. 2022b, Proc. SPIE, 12184, 121843Y Mawet, D. et al. 2018, Proc. SPIE, 10703, 1070306; Vigan, A. et al. 2018, Proc. SPIE 10702, 1070236

DOI:
10.18727/0722-6691/5315
ADS BibCode:
2023Msngr.190...58R
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
De Rosa, R.J.; Otarola, A.; Szeifert, T.; Smoker, J.; Selman, F.; Mehner, A.; Bian, F.; Sedaghati, E.; Seidel, J.V.; Smette, A.; de Wit, W.-J.
AA(ESO) AB(ESO) AC(ESO) AD(ESO; UK Astronomy Technology Centre, Royal Observatory, Edinburgh, UK) AE(ESO) AF(ESO) AG(ESO) AH(ESO) AI(ESO) AJ(ESO) AK(ESO)
Abstract:
The Hunga Tonga–Hunga Ha‘apai volcano erupted on 15 January 2022 with an energy equivalent to around 61 megatons of TNT. The explosion was bigger than any other volcanic eruption so far in the 21st century. Huge quantities of particles, including dust and water vapour, were released into the atmosphere. We present the results of a preliminary study of the effects of the explosion on observations taken at Paranal Observatory using a range of instruments. These effects were not immediately transitory in nature, and a year later stunning sunsets are still being seen at Paranal.
References:
Behringer, W. 2019, Tambora and the Year without a Summer: How a Volcano Plunged the World into Crisis (Medford, MA: Polity Press) Burki, G. et al. 1995a, The Messenger, 80, 34; Burki, G. et al. 1995b, A&AS, 112, 383; D’Arcy Wood, G. 2014, Tambora: The Eruption That Changed the World (Princeton: Princeton University Press) Diaz, J. S. & Rigby, S. E. 2022, Shock Waves, 32, 553; Freudling, W. et al. 2007, The Messenger, 128, 13; Grothues, H.-G. & Gochermann, J. 1992, The Messenger, 68, 43; Harrison, G. 2022, Weather, 77, 87; Kerber, F. et al. 2012, Proc. SPIE, 8446, 84463N Legras, B. et al. 2022, Atmos. Chem. Phys., 22, 14957; Millán, L. et al. 2022, Geophys. Res. Lett., 49, 99381; Moreno, H. & Stock, J. 1964, PASP, 76, 55; Proud, S. R., Prata, A. T. & Schmauß, S. 2022, Science, 378, 554; Royal Society 1888, The Eruption of Krakatoa: And Subsequent Phenomena (London, Trübner & Company) Rufener, F. 1986a, The Messenger, 44, 32; Rufener, F. 1986b, A&A, 165, 275; Paine, S. 2022, The am atmopsheric model (v. 12.2), https://doi.org/10.5281/zenodo.6774376

DOI:
10.18727/0722-6691/5316
ADS BibCode:
2023Msngr.190...63J
Section:
Astronomical News
Author(s)/Affiliation(s):
Jerabkova, T.; Patat, F.; Primas, F.; Dorigo, D.; Sogni, F.; Astolfi, L.; Bierwirth, T.; Prümm, M.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO)
Abstract:
The European Southern Observatory (ESO) implemented a new paradigm called Distributed Peer Review (DPR) as part of its proposal evaluation process in Period 110. Under DPR, Principal Investigators who submit proposals agree to review a certain number of proposals submitted by their peers and accept that their own proposal(s) are reviewed by their peers who have also submitted proposals in the same cycle. This article presents a brief overview of the DPR process at ESO, and its outcomes based on data from periods 110 and 111.
References:
Andersen, M. 2020, Nature Astronomy, 4, 646; Faez, A., Dickerson, J. P. & Fuge, M. 2017, Proceedings of the Twenty-Sixth International Joint Conference on Artificial Intelligence, 35; Kerzendorf, W. E. et al. 2020, Nature Astronomy, 4, 711; Merrifield, M. R. & Saari, D. G. 2009, A&G, 50, 4.16; Meyer, J. D. et al. 2022, Bull. Am. Ast. Soc., in press Patat, F. 2018, The Messenger, 173, 7; Patat, F. et al. 2019, The Messenger, 177, 3; Primas, F. et al. 2019, The Messenger, 176, 41; Stelmakh, I., Shah, N. B. & Singh, A. 2018, arXiv:1806.06237

DOI:
10.18727/0722-6691/5317
ADS BibCode:
2023Msngr.190...67P
Section:
Astronomical News
Author(s)/Affiliation(s):
Paladini, C.; Tristram, K.R.W.; de Gregorio-Monsalvo, I.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
As part of the International Astronomical Union’s Hands-On Workshops (I-HOW) initiative, ESO Chile organised the first international Very Large Telescope Interferometer (VLTI) workshop in Vitacura. The main goal was to train young scientists from Latin American countries in accessing, analysing and using VLTI archival data for their research projects. Through a series of lectures on interferometry and instrumentation, science, and soft skills, followed by practical hands-on sessions, the attendees were given the tools they needed to start using VLTI data for their own research. The workshop provided the perfect environment in which to build a network between VLTI specialists and future users and it furnished a great experience for all the participants, students, teachers and organisers alike.
References:
Garcia, P. 2009, The Messenger, 135, 50; Millour, F. et al. 2021, The Messenger, 185, 28

DOI:
10.18727/0722-6691/5318
ADS BibCode:
2023Msngr.190...70E
Section:
Astronomical News
Author(s)/Affiliation(s):
Rivera, C.G.; Ginolfi, M.; Seidel, J.V.; Abdul-Masih, M.