Project leaders: Bertoldi, Frank (AIfA); Riechers, Dominik (PH1)
Project C2 complements project C1 by measuring the dust-obscured fraction of star formation in galaxies at high redshift. By probing to three times lower luminosities and over larger areas than Herschel, it will trace the star formation history of the universe and find the most massive starburst galaxies in the universe. While C1 focuses on in-depth studies of key samples of galaxies, C2 pro- vides the necessary context by studying large, comprehensive statistical samples of hundreds of thousands of galaxies and their environments, addressing potential effects of sample and cosmic variance. In particular, these studies will: (1) lead to robust constraints on the the luminosities of bright submillimeter sources from z = 1 out to z > 5; (2) statistically constrain the cosmic star formation history out to z ∽ 5; (3) study the impact of environment on the population of high luminosity dusty star-forming galaxies; (4) reveal their evolutionary link to today’s ellipticals; (5) study “exotic” sources, such as protoclusters and strongly lensed sources. This will be achieved by deploying unprecedentedly large, multi-color (sub-)millimeter cameras on the most powerful single-dish survey telescopes at these wavelengths, in particular the newly-constructed CCAT-prime observatory, in which we are a major partner.
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title = {[C II]-deficit caused by self-absorption in an ionized carbon-filled bubble in RCW79},
author = {Eduard Keilmann and Simon Dannhauer and Slawa Kabanovic and Nicola Schneider and Volker Ossenkopf-Okada and Robert Simon and Lars Bonne and Paul F. Goldsmith and Rolf Güsten and Annie Zavagno and Jürgen Stutzki and Dominik Riechers and Markus Röllig and Juan L. Verbena and Alexander G. G. M. Tielens},
url = {https://arxiv.org/abs/2504.08976},
doi = {10.48550/arXiv.2504.08976},
year = {2025},
date = {2025-01-01},
urldate = {2025-01-01},
journal = {A&A},
keywords = {},
pubstate = {published},
tppubtype = {article}
}
@article{2024arXiv241202557C,
title = {Dust emission from the bulk of galaxies at the Epoch of Reionization},
author = {L. Ciesla and S. Adscheid and B. Magnelli and M. Boquien and N. Laporte and M. Bethermin and C. Carvajal and E. Schinnerer and D. Liu},
doi = {10.48550/arXiv.2412.02557},
year = {2024},
date = {2024-12-01},
journal = {arXiv e-prints},
pages = {arXiv:2412.02557},
keywords = {},
pubstate = {published},
tppubtype = {article}
}
@article{2024Natur.636...69T,
title = {In situ spheroid formation in distant submillimetre-bright galaxies},
author = {Qing-Hua Tan and Emanuele Daddi and Benjamin Magnelli and Camila A. Correa and Frédéric Bournaud and Sylvia Adscheid and Shao-Bo Zhang and David Elbaz and Carlos Gómez-Guijarro and Boris S. Kalita and Daizhong Liu and Zhaoxuan Liu and Jérôme Pety and Annagrazia Puglisi and Eva Schinnerer and John D. Silverman and Francesco Valentino},
doi = {10.1038/s41586-024-08201-6},
year = {2024},
date = {2024-12-01},
journal = {Nature},
volume = {636},
number = {8041},
pages = {69-74},
keywords = {},
pubstate = {published},
tppubtype = {article}
}
@article{2024A&A...688A..55M,
title = {A^{3}COSMOS: Measuring the cosmic dust-attenuated star formation rate density at 4 < z < 5},
author = {Benjamin Magnelli and Sylvia Adscheid and Tsan-Ming Wang and Laure Ciesla and Emanuele Daddi and Ivan Delvecchio and David Elbaz and Yoshinobu Fudamoto and Shuma Fukushima and Maximilien Franco and Carlos Gómez-Guijarro and Carlotta Gruppioni and Eric F. Jiménez-Andrade and Daizhong Liu and Pascal Oesch and Eva Schinnerer and Alberto Traina},
doi = {10.1051/0004-6361/202450081},
year = {2024},
date = {2024-08-01},
urldate = {2024-08-01},
journal = {A&A},
volume = {688},
pages = {A55},
keywords = {},
pubstate = {published},
tppubtype = {article}
}
@article{2024A&A...685A...1A,
title = {A^{3}COSMOS and A^{3}GOODSS: Continuum source catalogues and multi-band number counts},
author = {Sylvia Adscheid and Benjamin Magnelli and Daizhong Liu and Frank Bertoldi and Ivan Delvecchio and Carlotta Gruppioni and Eva Schinnerer and Alberto Traina and Matthieu Béthermin and Athanasia Gkogkou},
doi = {10.1051/0004-6361/202348407},
year = {2024},
date = {2024-05-01},
urldate = {2024-05-01},
journal = {A&A},
volume = {685},
pages = {A1},
keywords = {},
pubstate = {published},
tppubtype = {article}
}
An, Simpson, Smail, Swinbank, Ma, Liu, 33 co-authors including, and Bertoldi, “Multi-wavelength Prop- erties of Radio- and Machine-learning-identified Counterparts to Submillimeter Sources in S2COSMOS”, ApJ 886, 48 (2019).
Aravena, Decarli, Walter, Da Cunha, 30 co-authors including, Riechers, Weiss, and Bertoldi, “The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: Continuum Number Counts, Resolved 1.2 mm Extragalactic Background, and Properties of the Faintest Dusty Star-forming Galaxies”, ApJ833, 68 (2016).
Bertoldi, Carilli, Aravena, Schinnerer, Voss, Smolcic, Jahnke, Scoville, et al., “COSBO: The MAMBO 1.2 Millimeter Imaging Survey of the COSMOS Field”, ApJS 172, 132 (2007).
Bussmann, Riechers, Fialkov, Scudder, Hayward, Cowley, Bock, Calanog, et al., “HerMES: ALMA Imaging of Herschel-selected Dusty Star-forming Galaxies”, ApJ 812, 43 (2015).
Choi, Austermann, Basu, Battaglia, Bertoldi, Chung, Cothard, Duff, et al., “Sensitivity of the Prime-Cam Instrument on the CCAT-Prime Telescope”, Journal of Low Temperature Physics 199, 1089 (2020).
Gómez-Guijarro, Riechers, Pavesi, Magdis, Leung, Valentino, Toft, Aravena, et al., “Confirming Her- schel Candidate Protoclusters from ALMA/VLA CO Observations”, ApJ 872, 117 (2019).
Magnelli, Boogaard, Decarli, Gónzalez-López, 23 co-authors including, Bertoldi, Riechers, and Weiss, “The ALMA Spectroscopic Survey in the HUDF: The Cosmic Dust and Gas Mass Densities in Galaxies up to z ⇠ 3”, ApJ 892, 66 (2020).
Riechers, Bradford, Clements, Dowell, Pérez-Fournon, Ivison, Bridge, Conley, et al., “A dust-obscured massive maximum-starburst galaxy at a redshift of 6.34”, Nature 496, 329 (2013).
Riechers, Leung, Ivison, Pérez-Fournon, Lewis, Marques-Chaves, Oteo, Clements, et al., “Rise of the Titans: A Dusty, Hyper-luminous “870 μm Riser” Galaxy at z ⇠ 6”, ApJ 850, 1 (2017).
Walter, Carilli, Neeleman, Decarli, Popping, Somerville, Aravena, Bertoldi, et al., “The Evolution of the Baryons Associated with Galaxies Averaged over Cosmic Time and Space”, ApJ 902, 111 (2020).
Day 1
25.03.2025
Lecture Hall
seminar room 1
seminar room 2
seminar room3
08.00
Departure Cologne
08.45
Departure Bonn
9.45-10.30
Registration / welcome coffee
Chair: Lucas Labadie
10.30 – 10.45
Stefanie Walch-Gassner
Welcome
10:45 – 11:00
Stefanie Walch-Gassner
CRC 1601 – the big questions
11:00 – 11:25
Progress on project area A
11:25 – 11:50
Progress on project area B
11:50 – 12:15
Progress on project area C
12:15 – 12:25
Volker Ossenkopf-Okada
Sustainability Board
12.30 – 13.30
Lunchbuffet
Chair:
13:30 – 13:45
Working group ogrzanizers: Chinmaya Nagar, Divita Gupta, Ina Galić, Masato Kobayashi, Simon Dannhauer, Vittoria Brugaletta, Wonju Kim, and Zein Bazzi
Achievement and progress report from SFB working groups.
13:45 – 14:00
Planning of discussion rounds
14.00 – 15.00
Student Meeting (incl. Student Council)
PI meeting
Discussion groups
Discussion groups
15:00 – 16:00
Discussion groups
PI meeting
Discussion groups
Discussion groups
16:00 – 16:30:00
Coffee break
Chair:
16.00 – 16.25
Petra Fackendahl, Isabelle Breloy
Report from TP Z & Financial
16:30 – 17:50
all
Discussion groups
Discussion groups
Discussion groups
Discussion groups
18.00
Dinner
Day 2
26.03.2025
Lecture Hall
seminar room 1
seminar room 2
seminar room3
08.00 – 09.00
Breakfast
Chair:
9:00 – 9:30
TBD
Wrap up of day 1, results of discussion groups
9:30 – 10:00
Discussion groups
Sustainability Board Meeting
Diversity Board Meeting
Executive Board Meeting
10:00 – 10:30
Discussion groups
Discussion groups
Discussion groups
10:30 – 11:00
Coffee Break
11.00-15.00
Hiking
Chair: Dominik Riechers
15:00 – 16:00
all
Poster presentations (2min)
16:00 – 17:00
Coffee Break & Poster reception
17:00 – 18:30
all
Discussion groups
Discussion groups
Discussion groups
Discussion groups
19:00 – 24:00
Dinnerparty
Day 3
27.03.2025
Lecture Hall
08.00 – 09.00
Breakfast
Chair:
9:00 – 10:30
TBD
Wrap up of day 2, results of discussion groups
10.30 – 11.00
Coffee Break
Chair:
11.00 – 11.15
Report by the Sustainability Board
11.15 – 11.30
Report by the Student Council
11.30 – 11.45
Report by the Diversity Board
12:10 – 12:25
Summary
12.30 – 13.30
Lunchbuffet
13.30 – 15.30
Members Assembly (obligatory)
16:00
Departure
Project Area C
The observational projects C1 to C3 and related theory projects C5 and C6 cover observations of the habitats of massive stars from tens of parsec to Mpc scales in “typical”, starburst, and AGN host galaxies over 13 billion years of the history of the universe, critically complementing the other project areas in scales, diversity of environments, and cosmic time. A combination of the most sensitive facilities like ALMA and JWST with new wide-field observatories like FYST/CCAT-prime make it possible to reach both the level of detail and statistical robustness to push these studies to the next level. To prepare for the future, critical detector and readout technology development is delivered by projects C7 and C8, as necessary to build a new generation of instruments that speed up the FYST/CCAT-prime surveys in C2 and C3 by an order of magnitude in the later funding phases. In tandem with these developments, the laboratory spectroscopy and modelling of molecular ions done in C4 are critical to fully exploit a suite of new key tracers of massive star-forming environments in the Early Universe, as targeted in C1.
Image credits: C3/C6 from Karoumpis et al. 2022; C4 from Töpfer et al. 2020; C7 provided by N. Honingh; C8 from Klein et al. 2012; Galaxy composite for C1, C2 and C5 is a composite image of NGC 628 with ALMA (orange) and Hubble (blue) data provided by NRAO/AUI/NSF, B. Saxton: ALMA (ESO/NAOJ/NRAO), NASA/Hubble; for the connection to project areas A and B we show Orion.
Project Area B
B studies the habitats of massive stars on galactic scales. We show a portion of the Galactic disc plane as observed with Spitzer in purple and with ATLASGAL in orange and the corresponding molecular clouds identified in SEDIGISM (credit: Wyrowski; Duarte-Cabral et al. 2021) showcasing the Milky Way part of projects B1 & B2. In B1, parsec-scale observations of Milky Way massive clumps are combined with synthetic observations based on high-resolution simulations7. In B2, high-feedback regions are studied (credit: Simon). B3 will study massive star habitats in nearby galaxies (credit: Bigiel/PHANGS). B2 and B3 make use of the new CHAI instrument to be installed at FYST/CCAT-prime. The low-frequency channel of CHAI is used to study the whole Galactic disc, the Magellanic Clouds, and nearby galaxies in CO (J = 4 – 3) and [CI]. The high-frequency channel of CHAI is developed in the first CRC funding period in B7 (credit: Graf/Honingh). B4 studies the impact of magnetic fields in different environments using different techniques (e.g. dust polarisation; the synthetic map shown is taken from Seifried et al. 2019). B5 studies the late stages of massive star habitats (supernova remnants) using a new combination observations towards pulsar sight- lines (credit: Yao et al. 2021) with state-of-the-art simulations of the multi-phase interstellar medium that include supernovae (see also B6; credit: Walch; Rathjen et al. 2021). In B8, the (far-)infrared spectra of molecular anions (e.g. PAHs) are recorded in the laboratory in order to better constrain the observed emission of massive star habitats (credit: Schlemmer)
Image credits: B1 background: ESO/APEX/ATLASGAL consortium/NASA/GLIMPSE consortium/ESA/Planck.
Project Area A
Habitats of massive stars at high resolution. We combine different methodological pillars. Three observational projects study different phases of massive star formation at high resolution. We include hot molecular cores (A1), massive star formation in different galactic habitats (A2), and the infrared view on massive stars in different environments (A3). These observational efforts are combined with laboratory astrophysics (A4) measuring the spectra of complex molecules and high-resolution 3D simulations of massive star formation and star cluster evolution (A5), as well as detailed modelling of PDRs and dust (A6) needed to interpret the observations.
Image credits: background: Gaia’s view of the Milky Way (credit: ESO/Gaia/DPAC). Foreground: (A1, A2 and A4) ALMA emission spectrum of a hot core and a synthetic, laboratory-based spectrum mirrored in absorption (credit: Endres et al. 2021); (A1) image of the Large Magellanic Cloud (LMC), with the zoom-in showing the ALMA 1.3 mm continuum emission of a cluster-forming region in the LMC (credit: Hamedani Golshan); (A2) ALMA observations of a super-stellar cluster progenitor in Sgr B2 with converging dense filaments and an expanding molecular outflow (credit: Schwörer, Sánchez-Monge); (A3) collage of massive star binaries in Orion (credit: GRAVITY collaboration, M. Karl); (A5) massive star formation simulation with the MHD code FLASH (credit: Klepitko, Walch); (A6) Orion Bar in HCO+ with PDR model description (credit: Röllig, Ossenkopf-Okada).
image credit
1_SFB2023_overview_title_asm: SgrB2: Schwörer, Sánchez-Monge (A); Orion KL: Bally et al. 2017 (A); M16: NASA, Jeff Hester, and Paul Scowen (Arizona State University) (A-B); Crab nebula: NASA, ESA, J. Hester and A. Loll (Arizona State University) (B); Antennae: ALMA (ESO/NAOJ/NRAO). Visible light image: the NASA/ESA Hubble Space Telescope (A); M82: NASA/JPL-Caltech/STScI/CXC/UofA/ESA/AURA/JHU (B-C); Universe: J.Neidel/J.Onorbe/MPIA (C).
