Zobrazeno 1 - 10
of 3 995
pro vyhledávání: '"van der Wel A"'
Autor:
Kapoor, Anand Utsav, Baes, Maarten, van der Wel, Arjen, Gebek, Andrea, Camps, Peter, Smith, Aaron, Boquien, Médéric, Andreadis, Nick, Vicens, Sebastien
Current galaxy formation simulations often approximate star-formation, necessitating models of star-forming regions to produce observables. In the first paper of the series, we introduced TODDLERS, a time-resolved model of UV-mm emission from star-fo
Externí odkaz:
http://arxiv.org/abs/2410.01067
Autor:
Benton, Chloë E., Nelson, Erica J., Miller, Tim B., Bezanson, Rachel, Gibson, Justus, Hartley, Abigail I, Martorano, Marco, Price, Sedona H., Suess, Katherine A., van der Wel, Arjen, van Dokkum, Pieter, Weaver, John R., Whitaker, Katherine E.
Publikováno v:
2024 ApJL 974 L28
Hubble Space Telescope imaging shows that most star-forming galaxies at cosmic noon -- the peak of cosmic star formation history -- appear disk-dominated, leaving the origin of the dense cores in their quiescent descendants unclear. With the James We
Externí odkaz:
http://arxiv.org/abs/2409.08328
Autor:
Chastenet, Jérémy, De Looze, Ilse, Relaño, Monica, Dale, Daniel A., Williams, Thomas G., Bianchi, Simone, Xilouris, Emmanuel M., Baes, Maarten, Bolatto, Alberto D., Boyer, Martha L., Casasola, Viviana, Clark, Christopher J. R., Fraternali, Filippo, Fritz, Jacopo, Galliano, Frédéric, Glover, Simon C. O., Gordon, Karl D., Hirashita, Hiroyuki, Kennicutt, Robert, Nagamine, Kentaro, Kirchschlager, Florian, Klessen, Ralf S., Koch, Eric W., Levy, Rebecca C., McCallum, Lewis, Madden, Suzanne C., McLeod, Anna F., Meidt, Sharon E., Mosenkov, Aleksandr V., Richie, Helena M., Saintonge, Amélie, Sandstrom, Karin M., Schneider, Evan E., Sivkova, Evgenia E., Smith, J. D. T., Smith, Matthew W. L., van der Wel, Arjen, Walch, Stefanie, Walter, Fabian, Wood, Kenneth
Publikováno v:
A&A 690, A348 (2024)
We present new JWST observations of the nearby, prototypical edge-on, spiral galaxy NGC 891. The northern half of the disk was observed with NIRCam in its F150W and F277W filters. Absorption is clearly visible in the mid-plane of the F150W image, alo
Externí odkaz:
http://arxiv.org/abs/2408.08026
Autor:
Cheng, Chloe M., Kriek, Mariska, Beverage, Aliza G., van der Wel, Arjen, Bezanson, Rachel, D'Eugenio, Francesco, Franx, Marijn, Piña, Pavel E. Mancera, Nersesian, Angelos, Slob, Martje, Suess, Katherine A., van Dokkum, Pieter G., Wu, Po-Feng, Gallazzi, Anna, Zibetti, Stefano
We present spatially resolved, simple stellar population equivalent ages, stellar metallicities, and abundance ratios for 456 massive ($10.3\lesssim\log(\mathrm{M}_*/\mathrm{M}_\odot)\lesssim11.8$) quiescent galaxies at $0.6\lesssim z\lesssim1.0$ fro
Externí odkaz:
http://arxiv.org/abs/2407.10974
Autor:
D'Eugenio, Francesco, Colless, Matthew, van der Wel, Arjen, Vaughan, Sam P., Said, Khaled, van de Sande, Jesse, Bland-Hawthorn, Joss, Bryant, Julia J., Croom, Scott M., Lopez-Sanchez, Angel R., Lorente, Nuria P. F., Maiolino, Roberto, Taylor, Edward N.
We use deep spectroscopy from the SAMI Galaxy Survey to explore the precision of the fundamental plane of early-type galaxies (FP) as a distance indicator for future single-fibre spectroscopy surveys. We study the optimal trade-off between sample siz
Externí odkaz:
http://arxiv.org/abs/2406.17842
Autor:
Martorano, Marco, van der Wel, Arjen, Baes, Maarten, Bell, Eric F., Brammer, Gabriel, Franx, Marijn, Nersesian, Angelos
Publikováno v:
The Astrophysical Journal (2024), Volume 972, Number 2
We present the galaxy stellar mass - size relation in the rest-frame near-IR ($1.5~\mu{\text{m}}$) and its evolution with redshift up to $z=2.5$. S\'ersic profiles are measured for $\sim$ $26\,000$ galaxies with stellar masses $M_\star > 10^9~{\text{
Externí odkaz:
http://arxiv.org/abs/2406.17756
Autor:
Nedkova, Kalina V., Häußler, Boris, Marchesini, Danilo, Brammer, Gabriel B., Feinstein, Adina D., Johnston, Evelyn J., Kartaltepe, Jeyhan S., Koekemoer, Anton M., Martis, Nicholas S., Muzzin, Adam, Rafelski, Marc, Shipley, Heath V., Skelton, Rosalind E., Stefanon, Mauro, van der Wel, Arjen, Whitaker, Katherine E.
Using deep imaging from the CANDELS and HFF surveys, we present bulge+disc decompositions with GalfitM for $\sim$17,000 galaxies over $0.2 \leq z\leq 1.5$. We use various model parameters to select reliable samples of discs and bulges, and derive the
Externí odkaz:
http://arxiv.org/abs/2406.14613
Autor:
Clausen, Maike, Whitaker, Katherine E., Momcheva, Ivelina, Cutler, Sam E., Suess, Katherine A., Weaver, John R., Miller, Tim, van der Wel, Arjen, Wuyts, Stijn, Wake, David, van Dokkum, Pieter, Bezanson, Rachel S., Brammer, Gabriel, Franx, Marijn, Nelson, Erica J., Schreiber, Natasha M. Foerster
We present a study of the growth of the quiescent galaxy population between 0.5 < z < 3 by tracing the number density and structural evolution of a sample of 4518 old and 583 young quiescent galaxies with log($M_*$/$M_{\odot}$)>10.4, selected from th
Externí odkaz:
http://arxiv.org/abs/2405.09354
Autor:
Gebek, Andrea, Trčka, Ana, Baes, Maarten, Martorano, Marco, Pillepich, Annalisa, Kapoor, Anand Utsav, Nersesian, Angelos, van der Wel, Arjen
We apply the 3D dust radiative transfer code SKIRT to the low-redshift ($z\leq0.1$) galaxy population in the TNG100 cosmological simulation, the fiducial run of the IllustrisTNG project. We compute global fluxes and spectral energy distributions (SED
Externí odkaz:
http://arxiv.org/abs/2405.04925
Autor:
Baes, Maarten, Mosenkov, Aleksandr, Kelly, Raymond, Abdurro'uf, Andreadis, Nick, Tulu, Sena Bokona, Camps, Peter, Emana, Abdissa Tassama, Fritz, Jacopo, Gebek, Andrea, Kovacic, Inja, La Marca, Antonio, Martorano, Marco, Nersesian, Angelos, Rodriguez-Gomez, Vicente, Tortora, Crescenzo, Trcka, Ana, Meulen, Bert Vander, van der Wel, Arjen, Wang, Lingyu
Galaxy sizes correlate with many other important properties of galaxies, and the cosmic evolution of galaxy sizes is an important observational diagnostic for constraining galaxy evolution models. The effective radius is probably the most widely used
Externí odkaz:
http://arxiv.org/abs/2401.04225