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195 results on '"Daddi, E."'

2. Noema formIng Cluster survEy (NICE): Discovery of a starbursting galaxy group with a radio-luminous core at z = 3.95

Author

Zhou, L., primary, Wang, T., additional, Daddi, E., additional, Coogan, R., additional, Sun, H., additional, Xu, K., additional, Arumugam, V., additional, Jin, S., additional, Liu, D., additional, Lu, S., additional, Sillassen, N., additional, Wang, Y., additional, Shi, Y., additional, Zhang, Z., additional, Tan, Q., additional, Gu, Q., additional, Elbaz, D., additional, Le Bail, A., additional, Magnelli, B., additional, Gómez-Guijarro, C., additional, d’Eugenio, C., additional, Magdis, G., additional, Valentino, F., additional, Ji, Z., additional, Gobat, R., additional, Delvecchio, I., additional, Xiao, M., additional, Strazzullo, V., additional, Finoguenov, A., additional, Schinnerer, E., additional, Rich, R. M., additional, Huang, J., additional, Dai, Y., additional, Chen, Y., additional, Gao, F., additional, Yang, T., additional, and Hao, Q., additional

Published
2024
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3. Identifying the reddest high-redshift galaxies in the Euclid Deep Fields with gradient-boosted trees

Author

Signor, T., primary, Rodighiero, G., additional, Bisigello, L., additional, Bolzonella, M., additional, Caputi, K. I., additional, Daddi, E., additional, De Lucia, G., additional, Enia, A., additional, Gabarra, L., additional, Gruppioni, C., additional, Humphrey, A., additional, La Franca, F., additional, Mancini, C., additional, Pozzetti, L., additional, Serjeant, S., additional, Spinoglio, L., additional, van Mierlo, S. E., additional, Andreon, S., additional, Auricchio, N., additional, Baldi, M., additional, Bardelli, S., additional, Battaglia, P., additional, Bender, R., additional, Bodendorf, C., additional, Bonino, D., additional, Branchini, E., additional, Brescia, M., additional, Brinchmann, J., additional, Camera, S., additional, Capobianco, V., additional, Carbone, C., additional, Carretero, J., additional, Casas, S., additional, Castellano, M., additional, Cavuoti, S., additional, Cimatti, A., additional, Cledassou, R., additional, Congedo, G., additional, Conselice, C. J., additional, Conversi, L., additional, Copin, Y., additional, Corcione, L., additional, Courbin, F., additional, Courtois, H. M., additional, Da Silva, A., additional, Degaudenzi, H., additional, Di Giorgio, A. M., additional, Dinis, J., additional, Dubath, F., additional, Dupac, X., additional, Dusino, S., additional, Ealet, A., additional, Farina, M., additional, Farrens, S., additional, Ferriol, S., additional, Fotopoulou, S., additional, Franceschi, E., additional, Galeotta, S., additional, Garilli, B., additional, Gillard, W., additional, Gillis, B., additional, Giocoli, C., additional, Grazian, A., additional, Grupp, F., additional, Guzzo, L., additional, Haugan, S. V. H., additional, Hook, I., additional, Hormuth, F., additional, Hornstrup, A., additional, Jahnke, K., additional, Kümmel, M., additional, Kermiche, S., additional, Kiessling, A., additional, Kilbinger, M., additional, Kitching, T., additional, Kurki-Suonio, H., additional, Ligori, S., additional, Lilje, P. B., additional, Lindholm, V., additional, Lloro, I., additional, Maino, D., additional, Maiorano, E., additional, Mansutti, O., additional, Marggraf, O., additional, Martinet, N., additional, Marulli, F., additional, Massey, R., additional, Medinaceli, E., additional, Melchior, M., additional, Mellier, Y., additional, Meneghetti, M., additional, Merlin, E., additional, Moresco, M., additional, Moscardini, L., additional, Munari, E., additional, Nichol, R. C., additional, Niemi, S.-M., additional, Padilla, C., additional, Paltani, S., additional, Pasian, F., additional, Pedersen, K., additional, Pettorino, V., additional, Pires, S., additional, Polenta, G., additional, Poncet, M., additional, Popa, L. A., additional, Raison, F., additional, Renzi, A., additional, Rhodes, J., additional, Riccio, G., additional, Romelli, E., additional, Roncarelli, M., additional, Rossetti, E., additional, Saglia, R., additional, Sapone, D., additional, Sartoris, B., additional, Schneider, P., additional, Schrabback, T., additional, Secroun, A., additional, Seidel, G., additional, Serrano, S., additional, Sirignano, C., additional, Sirri, G., additional, Stanco, L., additional, Surace, C., additional, Tallada-Crespí, P., additional, Teplitz, H. I., additional, Tereno, I., additional, Toledo-Moreo, R., additional, Torradeflot, F., additional, Tutusaus, I., additional, Valentijn, E. A., additional, Vassallo, T., additional, Veropalumbo, A., additional, Wang, Y., additional, Weller, J., additional, Williams, O. R., additional, Zoubian, J., additional, Zucca, E., additional, Burigana, C., additional, and Scottez, V., additional

Published
2024
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4. Euclid: Identifying the reddest high-redshift galaxies in the Euclid Deep Fields with gradient-boosted trees.

Author

Signor, T., Rodighiero, G., Bisigello, L., Bolzonella, M., Caputi, K. I., Daddi, E., De Lucia, G., Enia, A., Gabarra, L., Gruppioni, C., Humphrey, A., La Franca, F., Mancini, C., Pozzetti, L., Serjeant, S., Spinoglio, L., van Mierlo, S. E., Andreon, S., Auricchio, N., and Baldi, M.

Subjects
GALACTIC redshift, REDSHIFT, STANDARD deviations, GALACTIC evolution, STAR formation
Abstract

Context. ALMA observations show that dusty, distant, massive (M* ≳ 1011 M⊙) galaxies usually have a remarkable star-formation activity, contributing of the order of 25% of the cosmic star-formation rate density at z ≈ 3–5, and up to 30% at z ∼ 7. Nonetheless, they are elusive in classical optical surveys, and current near-IR surveys are able to detect them only in very small sky areas. Since these objects have low space densities, deep and wide surveys are necessary to obtain statistically relevant results about them. Euclid will potentially be capable of delivering the required information, but, given the lack of spectroscopic features at these distances within its bands, it is still unclear if Euclid will be able to identify and characterise these objects. Aims. The goal of this work is to assess the capability of Euclid, together with ancillary optical and near-IR data, to identify these distant, dusty, and massive galaxies based on broadband photometry. Methods. We used a gradient-boosting algorithm to predict both the redshift and spectral type of objects at high z. To perform such an analysis, we made use of simulated photometric observations that mimic the Euclid Deep Survey, derived using the state-of-the-art Spectro-Photometric Realizations of Infrared-selected Targets at all-z (SPRITZ) software. Results. The gradient-boosting algorithm was found to be accurate in predicting both the redshift and spectral type of objects within the simulated Euclid Deep Survey catalogue at z > 2, while drastically decreasing the runtime with respect to spectral-energy-distribution-fitting methods. In particular, we studied the analogue of HIEROs (i.e. sources selected on the basis of a red H − [4.5]> 2.25), combining Euclid and Spitzer data at the depth of the Deep Fields. These sources include the bulk of obscured and massive galaxies in a broad redshift range, 3 < z < 7. We find that the dusty population at 3 ≲ z ≲ 7 is well identified, with a redshift root mean squared error and catastrophic outlier fraction of only 0.55 and 8.5% (HE ≤ 26), respectively. Our findings suggest that with Euclid we will obtain meaningful insights into the impact of massive and dusty galaxies on the cosmic star-formation rate over time. [ABSTRACT FROM AUTHOR]

Published
2024
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6. The gas mass reservoir of quiescent galaxies at cosmic noon

Author

Blánquez, D., primary, Gómez-Guijarro, C., additional, Magdis, G. E., additional, Magnelli, B., additional, Gobat, R., additional, Daddi, E., additional, Franco, M., additional, Whitaker, K., additional, Valentino, F., additional, Adscheid, S., additional, Schinnerer, E., additional, Zanella, A., additional, Xiao, M., additional, Wang, T., additional, Liu, D., additional, Kokorev, V., additional, and Elbaz, D., additional

Published
2023
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7. The hidden side of cosmic star formation at z > 3

Author

Xiao, M.-Y., primary, Elbaz, D., additional, Gómez-Guijarro, C., additional, Leroy, L., additional, Bing, L.-J., additional, Daddi, E., additional, Magnelli, B., additional, Franco, M., additional, Zhou, L., additional, Dickinson, M., additional, Wang, T., additional, Rujopakarn, W., additional, Magdis, G. E., additional, Treister, E., additional, Inami, H., additional, Demarco, R., additional, Sargent, M. T., additional, Shu, X., additional, Kartaltepe, J. S., additional, Alexander, D. M., additional, Béthermin, M., additional, Bournaud, F., additional, Ciesla, L., additional, Ferguson, H. C., additional, Finkelstein, S. L., additional, Giavalisco, M., additional, Gu, Q.-S., additional, Iono, D., additional, Juneau, S., additional, Lagache, G., additional, Leiton, R., additional, Messias, H., additional, Motohara, K., additional, Mullaney, J., additional, Nagar, N., additional, Pannella, M., additional, Papovich, C., additional, Pope, A., additional, Schreiber, C., additional, and Silverman, J., additional

Published
2023
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9. A super-linear ‘radio-AGN main sequence’ links mean radio-AGN power and galaxy stellar mass since z ∼ 3

Author

Delvecchio, I., primary, Daddi, E., additional, Sargent, M. T., additional, Aird, J., additional, Mullaney, J. R., additional, Magnelli, B., additional, Elbaz, D., additional, Bisigello, L., additional, Ceraj, L., additional, Jin, S., additional, Kalita, B. S., additional, Liu, D., additional, Novak, M., additional, Prandoni, I., additional, Radcliffe, J. F., additional, Spingola, C., additional, Zamorani, G., additional, Allevato, V., additional, Rodighiero, G., additional, and Smolčić, V., additional

Published
2022
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11. Starbursts with suppressed velocity dispersion revealed in a forming cluster at z = 2.51

Author

Xiao, M.-Y., primary, Wang, T., additional, Elbaz, D., additional, Iono, D., additional, Lu, X., additional, Bing, L.-J., additional, Daddi, E., additional, Magnelli, B., additional, Gómez-Guijarro, C., additional, Bournaud, F., additional, Gu, Q.-S., additional, Jin, S., additional, Valentino, F., additional, Zanella, A., additional, Gobat, R., additional, Martin, S., additional, Brammer, G., additional, Kohno, K., additional, Schreiber, C., additional, Ciesla, L., additional, Yu, X.-L., additional, and Okumura, K., additional

Published
2022
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12. GOODS-ALMA 2.0 : starbursts in the main sequence reveal compact star formation regulating galaxy evolution prequenching

Author

Gómez-Guijarro, C., Elbaz, D., Xiao, M., Kokorev, V.I., Magdis, G.E., Magnelli, B., Daddi, E., Valentino, F., Sargent, M.T., Dickinson, M., Béthermin, M., Franco, M., Pope, A., Kalita, B.S., Ciesla, L., Demarco, R., Inami, H., Rujopakarn, W., Shu, X., Wang, T., Zhou, L., Alexander, D.M., Bournaud, F., Chary, R., Ferguson, H.C., Finkelstein, S.L., Giavalisco, M., Iono, D., Juneau, S., Kartaltepe, J.S., Lagache, G., Le Floc’h, E., Leiton, R., Leroy, L., Lin, L., Motohara, K., Mullaney, J., Okumura, K., Pannella, M., Papovich, C., and Treister, E.

Abstract

Compact star formation appears to be generally common in dusty star-forming galaxies (SFGs). However, its role in the framework set by the scaling relations in galaxy evolution remains to be understood. In this work we follow up on the galaxy sample from the GOODS-ALMA 2.0 survey, an ALMA blind survey at 1.1 mm covering a continuous area of 72.42 arcmin2 using two array configurations. We derived physical properties, such as star formation rates, gas fractions, depletion timescales, and dust temperatures for the galaxy sample built from the survey. There exists a subset of galaxies that exhibit starburst-like short depletion timescales, but they are located within the scatter of the so-called main sequence of SFGs. These are dubbed starbursts in the main sequence and display the most compact star formation and they are characterized by the shortest depletion timescales, lowest gas fractions, and highest dust temperatures of the galaxy sample, compared to typical SFGs at the same stellar mass and redshift. They are also very massive, accounting for ∼60% of the most massive galaxies in the sample (log(M*/M⊙) > 11.0). We find trends between the areas of the ongoing star formation regions and the derived physical properties for the sample, unveiling the role of compact star formation as a physical driver of these properties. Starbursts in the main sequence appear to be the extreme cases of these trends. We discuss possible scenarios of galaxy evolution to explain the results drawn from our galaxy sample. Our findings suggest that the star formation rate is sustained in SFGs by gas and star formation compression, keeping them within the main sequence even when their gas fractions are low and they are presumably on the way to quiescence.

Published
2022

13. The hidden side of cosmic star formation at z >3: Bridging optically dark and Lyman-break galaxies with GOODS-ALMA.

Author

Xiao, M.-Y., Elbaz, D., Gómez-Guijarro, C., Leroy, L., Bing, L.-J., Daddi, E., Magnelli, B., Franco, M., Zhou, L., Dickinson, M., Wang, T., Rujopakarn, W., Magdis, G. E., Treister, E., Inami, H., Demarco, R., Sargent, M. T., Shu, X., Kartaltepe, J. S., and Alexander, D. M.

Subjects
STAR formation, GALAXIES, DISTRIBUTION of stars, STELLAR mass, GALACTIC redshift, GAUSSIAN measures
Abstract

Our current understanding of the cosmic star formation history at z > 3 is primarily based on UV-selected galaxies (Lyman-break galaxies, i.e., LBGs). Recent studies of H-dropouts (HST-dark galaxies) have revealed that we may be missing a large proportion of star formation that is taking place in massive galaxies at z > 3. In this work, we extend the H-dropout criterion to lower masses to select optically dark or faint galaxies (OFGs) at high redshifts in order to complete the census between LBGs and H-dropouts. Our criterion (H > 26:5 mag & [4.5] < 25 mag) combined with a de-blending technique is designed to select not only extremely dust-obscured massive galaxies but also normal star-forming galaxies (typically E(B V) > 0:4) with lower stellar masses at high redshifts. In addition, with this criterion, our sample is not contaminated by massive passive or old galaxies. In total, we identified 27 OFGs at zphot > 3 (with a median of zmed = 4:1) in the GOODS-ALMA field, covering a wide distribution of stellar masses with log(MM) = 9:411:1 (with a median of log(Med/M) = 10.3). We find that up to 75% of the OFGs with log(M/M) = 9:510:5 were neglected by previous LBGs and H-dropout selection techniques. After performing an optical-to-millimeter stacking analysis of the OFGs, we find that rather than being limited to a rare population of extreme starbursts, these OFGs represent a normal population of dusty star-forming galaxies at z > 3. The OFGs exhibit shorter gas depletion timescales, slightly lower gas fractions, and lower dust temperatures than the scaling relation of typical star-forming galaxies. Additionally, the total star formation rate (SFRtot = SFRIR + SFRUV) of the stacked OFGs is much higher than the SFRcorr UV (SFRUV corrected for dust extinction), with an average SFRtot/SFRcorr UV = 8 ± 1, which lies above (~0.3 dex) the 16-84th percentile range of typical star-forming galaxies at 3 z 6. All of the above suggests the presence of hidden dust regions in the OFGs that absorb all UV photons, which cannot be reproduced with dust extinction corrections. The effective radius of the average dust size measured by a circular Gaussian model fit in the uv plane is Re(1:13 mm) = 1:01 ± 0:05 kpc. After excluding the five LBGs in the OFG sample, we investigated their contributions to the cosmic star formation rate density (SFRD). We found that the SFRD at z > 3 contributed by massive OFGs (log(MM) > 10:3) is at least two orders of magnitude higher than the one contributed by equivalently massive LBGs. Finally, we calculated the combined contribution of OFGs and LBGs to the cosmic SFRD at z = 45 to be 4 102 M yr1 Mpc3, which is about 0.15 dex (43%) higher than the SFRD derived from UV-selected samples alone at the same redshift. This value could be even larger, as our calculations were performed in a very conservative way. [ABSTRACT FROM AUTHOR]

Published
2023
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15. GOODS-ALMA 2.0 : source catalog, number counts, and prevailing compact sizes in 1.1 mm galaxies

Author

Gómez-Guijarro, C., Elbaz, D., Xiao, M., Béthermin, M., Franco, M., Magnelli, B., Daddi, E., Dickinson, M., Demarco, R., Inami, H., Rujopakarn, W., Magdis, G.E., Shu, X., Chary, R., Zhou, L., Alexander, D.M., Bournaud, F., Ciesla, L., Ferguson, H.C., Finkelstein, S.L., Giavalisco, M., Iono, D., Juneau, S., Kartaltepe, J.S., Lagache, G., Le Floc’h, E., Leiton, R., Lin, L., Motohara, K., Mullaney, J., Okumura, K., Pannella, M., Papovich, C., Pope, A., Sargent, M.T., Silverman, J.D., Treister, E., and Wang, T.

Abstract

Submillimeter/millimeter observations of dusty star-forming galaxies with the Atacama Large Millimeter/submillimeter Array (ALMA) have shown that dust continuum emission generally occurs in compact regions smaller than the stellar distribution. However, it remains to be understood how systematic these findings are. Studies often lack homogeneity in the sample selection, target discontinuous areas with inhomogeneous sensitivities, and suffer from modest uv coverage coming from single array configurations. GOODS-ALMA is a 1.1 mm galaxy survey over a continuous area of 72.42 arcmin2 at a homogeneous sensitivity. In this version 2.0, we present a new low resolution dataset and its combination with the previous high resolution dataset from the survey, improving the uv coverage and sensitivity reaching an average of σ = 68.4 μJy beam−1. A total of 88 galaxies are detected in a blind search (compared to 35 in the high resolution dataset alone), 50% at S/Npeak ≥ 5 and 50% at 3.5 ≤ S/Npeak ≤ 5 aided by priors. Among them, 13 out of the 88 are optically dark or faint sources (H- or K-band dropouts). The sample dust continuum sizes at 1.1 mm are generally compact, with a median effective radius of Re = 0.″10 ± 0.″05 (a physical size of Re = 0.73 ± 0.29 kpc at the redshift of each source). Dust continuum sizes evolve with redshift and stellar mass resembling the trends of the stellar sizes measured at optical wavelengths, albeit a lower normalization compared to those of late-type galaxies. We conclude that for sources with flux densities S1.1 mm > 1 mJy, compact dust continuum emission at 1.1 mm prevails, and sizes as extended as typical star-forming stellar disks are rare. The S1.1 mm < 1 mJy sources appear slightly more extended at 1.1 mm, although they are still generally compact below the sizes of typical star-forming stellar disks.

Published
2022

16. The effect of active galactic nuclei on the cold interstellar medium in distant star-forming galaxies

Author

Valentino, F., primary, Daddi, E., additional, Puglisi, A., additional, Magdis, G. E., additional, Kokorev, V., additional, Liu, D., additional, Madden, S. C., additional, Gómez-Guijarro, C., additional, Lee, M.-Y., additional, Cortzen, I., additional, Circosta, C., additional, Delvecchio, I., additional, Mullaney, J. R., additional, Gao, Y., additional, Gobat, R., additional, Aravena, M., additional, Jin, S., additional, Fujimoto, S., additional, Silverman, J. D., additional, and Dannerbauer, H., additional

Published
2021
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18. Three Lyman-α-emitting filaments converging to a massive galaxy group at z = 2.91: discussing the case for cold gas infall

Author

Daddi, E., primary, Valentino, F., additional, Rich, R. M., additional, Neill, J. D., additional, Gronke, M., additional, O’Sullivan, D., additional, Elbaz, D., additional, Bournaud, F., additional, Finoguenov, A., additional, Marchal, A., additional, Delvecchio, I., additional, Jin, S., additional, Liu, D., additional, Strazzullo, V., additional, Calabro, A., additional, Coogan, R., additional, D’Eugenio, C., additional, Gobat, R., additional, Kalita, B. S., additional, Laursen, P., additional, Martin, D. C., additional, Puglisi, A., additional, Schinnerer, E., additional, and Wang, T., additional

Published
2021
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19. The infrared-radio correlation of star-forming galaxies is stronglyM⋆-dependent but nearly redshift-invariant sincez∼ 4

Author

Delvecchio, I., primary, Daddi, E., additional, Sargent, M. T., additional, Jarvis, M. J., additional, Elbaz, D., additional, Jin, S., additional, Liu, D., additional, Whittam, I. H., additional, Algera, H., additional, Carraro, R., additional, D’Eugenio, C., additional, Delhaize, J., additional, Kalita, B. S., additional, Leslie, S., additional, Molnár, D. Cs., additional, Novak, M., additional, Prandoni, I., additional, Smolčić, V., additional, Ao, Y., additional, Aravena, M., additional, Bournaud, F., additional, Collier, J. D., additional, Randriamampandry, S. M., additional, Randriamanakoto, Z., additional, Rodighiero, G., additional, Schober, J., additional, White, S. V., additional, and Zamorani, G., additional

Published
2021
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21. GOODS-ALMA: Using IRAC and VLA to probe fainter millimeter galaxies

Author

Franco, M., primary, Elbaz, D., additional, Zhou, L., additional, Magnelli, B., additional, Schreiber, C., additional, Ciesla, L., additional, Dickinson, M., additional, Nagar, N., additional, Magdis, G., additional, Alexander, D. M., additional, Béthermin, M., additional, Demarco, R., additional, Daddi, E., additional, Wang, T., additional, Mullaney, J., additional, Inami, H., additional, Shu, X., additional, Bournaud, F., additional, Chary, R., additional, Coogan, R. T., additional, Ferguson, H., additional, Finkelstein, S. L., additional, Giavalisco, M., additional, Gómez-Guijarro, C., additional, Iono, D., additional, Juneau, S., additional, Lagache, G., additional, Lin, L., additional, Motohara, K., additional, Okumura, K., additional, Pannella, M., additional, Papovich, C., additional, Pope, A., additional, Rujopakarn, W., additional, Silverman, J., additional, and Xiao, M., additional

Published
2020
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22. GOODS-ALMA: The slow downfall of star formation in z = 2–3 massive galaxies

Author

Franco, M., primary, Elbaz, D., additional, Zhou, L., additional, Magnelli, B., additional, Schreiber, C., additional, Ciesla, L., additional, Dickinson, M., additional, Nagar, N., additional, Magdis, G., additional, Alexander, D. M., additional, Béthermin, M., additional, Demarco, R., additional, Daddi, E., additional, Wang, T., additional, Mullaney, J., additional, Sargent, M., additional, Inami, H., additional, Shu, X., additional, Bournaud, F., additional, Chary, R., additional, Coogan, R. T., additional, Ferguson, H., additional, Finkelstein, S. L., additional, Giavalisco, M., additional, Gómez-Guijarro, C., additional, Iono, D., additional, Juneau, S., additional, Lagache, G., additional, Lin, L., additional, Motohara, K., additional, Okumura, K., additional, Pannella, M., additional, Papovich, C., additional, Pope, A., additional, Rujopakarn, W., additional, Silverman, J., additional, and Xiao, M., additional

Published
2020
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23. GOODS-ALMA: Optically dark ALMA galaxies shed light on a cluster in formation at z = 3.5

Author

Zhou, L., primary, Elbaz, D., additional, Franco, M., additional, Magnelli, B., additional, Schreiber, C., additional, Wang, T., additional, Ciesla, L., additional, Daddi, E., additional, Dickinson, M., additional, Nagar, N., additional, Magdis, G., additional, Alexander, D. M., additional, Béthermin, M., additional, Demarco, R., additional, Mullaney, J., additional, Bournaud, F., additional, Ferguson, H., additional, Finkelstein, S. L., additional, Giavalisco, M., additional, Inami, H., additional, Iono, D., additional, Juneau, S., additional, Lagache, G., additional, Messias, H., additional, Motohara, K., additional, Okumura, K., additional, Pannella, M., additional, Papovich, C., additional, Pope, A., additional, Rujopakarn, W., additional, Shi, Y., additional, Shu, X., additional, and Silverman, J., additional

Published
2020
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24. Coevolution of black hole accretion and star formation in galaxies up to z = 3.5

Author

Carraro, R., primary, Rodighiero, G., additional, Cassata, P., additional, Brusa, M., additional, Shankar, F., additional, Baronchelli, I., additional, Daddi, E., additional, Delvecchio, I., additional, Franceschini, A., additional, Griffiths, R., additional, Gruppioni, C., additional, López-Navas, E., additional, Mancini, C., additional, Marchesi, S., additional, Negrello, M., additional, Puglisi, A., additional, Sani, E., additional, and Suh, H., additional

Published
2020
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25. CO emission in distant galaxies on and above the main sequence

Author

Valentino, F., primary, Daddi, E., additional, Puglisi, A., additional, Magdis, G. E., additional, Liu, D., additional, Kokorev, V., additional, Cortzen, I., additional, Madden, S., additional, Aravena, M., additional, Gómez-Guijarro, C., additional, Lee, M.-Y., additional, Le Floc’h, E., additional, Gao, Y., additional, Gobat, R., additional, Bournaud, F., additional, Dannerbauer, H., additional, Jin, S., additional, Dickinson, M. E., additional, Kartaltepe, J., additional, and Sanders, D., additional

Published
2020
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26. A hyper luminous starburst at z = 4.72 magnified by a lensing galaxy pair at z = 1.48

Author

Ciesla, L., primary, Béthermin, M., additional, Daddi, E., additional, Richard, J., additional, Diaz-Santos, T., additional, Sargent, M. T., additional, Elbaz, D., additional, Boquien, M., additional, Wang, T., additional, Schreiber, C., additional, Yang, C., additional, Zabl, J., additional, Fraser, M., additional, Aravena, M., additional, Assef, R. J., additional, Baker, A. J., additional, Beelen, A., additional, Boselli, A., additional, Bournaud, F., additional, Burgarella, D., additional, Charmandaris, V., additional, Côté, P., additional, Epinat, B., additional, Ferrarese, L., additional, Gobat, R., additional, and Ilbert, O., additional

Published
2020
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27. GOODS-ALMA: 1.1 mm galaxy survey

Author

Franco, M, Elbaz, D, Béthermin, M, Magnelli, B, Schreiber, C, Ciesla, L, Dickinson, M, Nagar, N, Silverman, J, Daddi, E, Alexander, D, Wang, T, Pannella, M, Le Floc’H, E, Pope, A, Giavalisco, M, Maury, A, Bournaud, F, Chary, R, Demarco, R, Ferguson, H, Finkelstein, S, Inami, H, Iono, D, Juneau, S, Lagache, G, Leiton, R, Lin, L, Magdis, G, Messias, H, Motohara, K, Mullaney, J, Okumura, K, Papovich, C, Pforr, J, Rujopakarn, W, Sargent, M, Shu, X, Zhou, L, School of Biological Sciences, Plymouth University, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut d'astrophysique spatiale (IAS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), National Optical Astronomy Observatory (NOAO), AUTRES, Department of Physics, Durham University, Institute of Biological and Environmental Sciences, (SFIRC), Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), Centre Hospitalier Régional Universitaire [Montpellier] (CHRU Montpellier), Departamento de Industrias, Universidad Técnica Federico Santa María, Av. España 1680, Valparaíso, Chile, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Steward observatory, University of Arizona, Observatório Astronómico de Lisboa, Institute of Astronomy, The University of Tokyo (UTokyo), Institut d'Electronique du Solide et des Systèmes (InESS), Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), NOAO, and The University of Tokyo

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA]
Abstract

Aims. We present a 69 arcmin2 ALMA survey at 1.1 mm, GOODS-ALMA, matching the deepest HST-WFC3 H-band part of the GOODS-South field. Methods. We tapered the 0″24 original image with a homogeneous and circular synthesized beam of 0″60 to reduce the number of independent beams – thus reducing the number of purely statistical spurious detections – and optimize the sensitivity to point sources. We extracted a catalog of galaxies purely selected by ALMA and identified sources with and without HST counterparts down to a 5σ limiting depth of H = 28.2 AB (HST/WFC3 F160W). Results. ALMA detects 20 sources brighter than 0.7 mJy at 1.1 mm in the 0″60 tapered mosaic (rms sensitivity σ ≃ 0.18 mJy beam−1) with a purity greater than 80%. Among these detections, we identify three sources with no HST nor Spitzer-IRAC counterpart, consistent with the expected number of spurious galaxies from the analysis of the inverted image; their definitive status will require additional investigation. We detect additional three sources with HST counterparts either at high significance in the higher resolution map, or with different detection-algorithm parameters ensuring a purity greater than 80%. Hence we identify in total 20 robust detections. Conclusions. Our wide contiguous survey allows us to push further in redshift the blind detection of massive galaxies with ALMA with a median redshift of z = 2.92 and a median stellar mass of M⋆ = 1.1 × 1011 M⊙. Our sample includes 20% HST-dark galaxies (4 out of 20), all detected in the mid-infrared with Spitzer-IRAC. The near-infrared based photometric redshifts of two of them (z ∼ 4.3 and 4.8) suggest that these sources have redshifts z > 4. At least 40% of the ALMA sources host an X-ray AGN, compared to ∼14% for other galaxies of similar mass and redshift. The wide area of our ALMA survey provides lower values at the bright end of number counts than single-dish telescopes affected by confusion.

Published
2019

28. HST grism spectroscopy of z ∼ 3 massive quiescent galaxies: Approaching the metamorphosis.

Author

D'Eugenio, C., Daddi, E., Gobat, R., Strazzullo, V., Lustig, P., Delvecchio, I., Jin, S., Cimatti, A., and Onodera, M.

Subjects
*GALAXIES, *ACTIVE galactic nuclei, *BLACK holes, *METAMORPHOSIS, *STAR formation, *STELLAR mass, *ACCRETION (Astrophysics), *X-ray binaries
Abstract

Tracing the emergence of the massive quiescent galaxy (QG) population requires the build-up of reliable quenched samples by distinguishing these systems from red, dusty star-forming sources. We present Hubble Space Telescope WFC3/G141 grism spectra of ten quiescent galaxy candidates selected at 2.5 < z < 3.5 in the COSMOS field. Spectroscopic confirmation for the whole sample is obtained within one to three orbits through the detection of strong spectral breaks and Balmer absorption lines. When their spectra are combined with optical to near-infrared photometry, star-forming solutions are formally rejected for the entire sample. Broad spectral indices are consistent with the presence of young A-type stars, which indicates that the last major episode of star formation has taken place no earlier than ∼300–800 Myr prior to observation. This confirms clues from their post-starburst UVJ colors. Marginalising over three different slopes of the dust attenuation curve, we obtain young mass-weighted ages and an average peak star formation rate (SFR) of ∼103 M⊙ yr−1 at zformation ∼ 3.5. Although mid- and far-IR data are too shallow to determine the obscured SFR on a galaxy-by-galaxy basis, the mean stacked emission from 3 GHz data constrains the level of residual-obscured SFR to be globally below 50 M⊙ yr−1, three times below the scatter of the coeval main sequence. Alternatively, the very same radio detection suggests a widespread radio-mode feedback by active galactic nuclei (AGN) four times stronger than in z ∼ 1.8 massive QGs. This is accompanied by a 30% fraction of X-ray luminous AGN with a black hole accretion rate per unit SFR enhanced by a factor of ∼30 with respect to similarly massive QGs at lower redshift. The average compact, high Sérsic index morphologies of the galaxies in this sample, coupled with their young mass-weighted ages, suggest that the mechanisms responsible for the development of a spheroidal component might be concomitant with (or preceding) those causing their quenching. [ABSTRACT FROM AUTHOR]

Published
2021
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29. The molecular gas content in obscured AGN at z > 1

Author

Perna, M., Sargent, M. T., Brusa, M., Daddi, E., Feruglio, C., Cresci, G., Lanzuisi, G., Lusso, E., Comastri, A., Coogan, R. T., D'Amato, Q., Gilli, R., Piconcelli, E., and Vignali, C.

Subjects
Astrophysics - Astrophysics of Galaxies, QB
Abstract

The standard AGN-galaxy co-evolutionary scenario predicts a phase of deeply buried supermassive black hole growth coexisting with a starburst (SB) before feedback phenomena deplete the cold molecular gas reservoir of the galaxy and an optically luminous QSO is revealed ('SB-QSO evolutionary sequence'). The aim of this work is to measure the cold gas reservoir of three highly obscured QSOs to test if their gas fraction is similar to that of sub-millimeter galaxies (SMGs), as expected by some models, and place these measurements in the context of the SB-QSO framework. We target CO(1-0) transition in BzK4892, a Compton Thick (CT) QSO at z=2.6, CO(1-0) in BzK8608 and CO(2-1) in CDF153, two highly obscured QSOs at z=2.5 and z=1.5, respectively. For all these targets, we place 3$\sigma$ upper limits on the CO, with $L'_{CO} < (1.5\div 2.8)\times 10^{10}$ K km/s pc$^2$. We also compare the molecular gas conditions of our targets with those of other systems at z>1, considering normal star forming galaxies and SMGs, unobscured and obscured AGN from the literature. For the AGN samples, we provide an updated and (almost) complete collection of targets with CO follow-up. BzK4892 displays a high star formation efficiency (SFE$=L_{IR}/L'_{CO}>410$ L$_{\odot}$/(K km s$^{-1}$ pc$^2$)) and a gas fraction $f_{gas}10$). From the comparison with literature data, we found that a) obscured AGN at z>1 are associated with higher SFE and lower $f_{gas}$ with respect to star forming galaxies; b) mildly and highly obscured active galaxies have comparable gas fractions; c) the SFE of CT and obscured AGN are similar to those of unobscured AGN. Within the SB-QSO framework, these findings could be consistent with a scenario where feedback can impact the host galaxy already from the early phases of the SB-QSO sequence., Comment: 20 pages, 7 figures, accepted for publication in A&A

Published
2018

32. Deciphering an evolutionary sequence of merger stages in infrared-luminous starburst galaxies atz∼ 0.7

Author

Calabrò, A., primary, Daddi, E., additional, Puglisi, A., additional, Oliva, E., additional, Gobat, R., additional, Cassata, P., additional, Amorín, R., additional, Arimoto, N., additional, Boquien, M., additional, Carraro, R., additional, Delvecchio, I., additional, Ibar, E., additional, Jin, S., additional, Juneau, S., additional, Liu, D., additional, Onodera, M., additional, Mannucci, F., additional, Méndez-Hernández, H., additional, Rodighiero, G., additional, Valentino, F., additional, and Zanella, A., additional

Published
2019
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33. GOODS-ALMA: 1.1 mm galaxy survey

Author

Franco, M., primary, Elbaz, D., additional, Béthermin, M., additional, Magnelli, B., additional, Schreiber, C., additional, Ciesla, L., additional, Dickinson, M., additional, Nagar, N., additional, Silverman, J., additional, Daddi, E., additional, Alexander, D. M., additional, Wang, T., additional, Pannella, M., additional, Le Floc’h, E., additional, Pope, A., additional, Giavalisco, M., additional, Maury, A. J., additional, Bournaud, F., additional, Chary, R., additional, Demarco, R., additional, Ferguson, H., additional, Finkelstein, S. L., additional, Inami, H., additional, Iono, D., additional, Juneau, S., additional, Lagache, G., additional, Leiton, R., additional, Lin, L., additional, Magdis, G., additional, Messias, H., additional, Motohara, K., additional, Mullaney, J., additional, Okumura, K., additional, Papovich, C., additional, Pforr, J., additional, Rujopakarn, W., additional, Sargent, M., additional, Shu, X., additional, and Zhou, L., additional

Published
2018
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35. Molecular gas content in obscured AGN at z > 1

Author

Perna, M., primary, Sargent, M. T., additional, Brusa, M., additional, Daddi, E., additional, Feruglio, C., additional, Cresci, G., additional, Lanzuisi, G., additional, Lusso, E., additional, Comastri, A., additional, Coogan, R. T., additional, D’Amato, Q., additional, Gilli, R., additional, Piconcelli, E., additional, and Vignali, C., additional

Published
2018
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36. Starbursts in and out of the star-formation main sequence

Author

Elbaz, D., primary, Leiton, R., additional, Nagar, N., additional, Okumura, K., additional, Franco, M., additional, Schreiber, C., additional, Pannella, M., additional, Wang, T., additional, Dickinson, M., additional, Díaz-Santos, T., additional, Ciesla, L., additional, Daddi, E., additional, Bournaud, F., additional, Magdis, G., additional, Zhou, L., additional, and Rujopakarn, W., additional

Published
2018
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38. Molecular outflow and feedback in the obscured quasar XID2028 revealed by ALMA

Author

Brusa, M., primary, Cresci, G., additional, Daddi, E., additional, Paladino, R., additional, Perna, M., additional, Bongiorno, A., additional, Lusso, E., additional, Sargent, M. T., additional, Casasola, V., additional, Feruglio, C., additional, Fraternali, F., additional, Georgiev, I., additional, Mainieri, V., additional, Carniani, S., additional, Comastri, A., additional, Duras, F., additional, Fiore, F., additional, Mannucci, F., additional, Marconi, A., additional, Piconcelli, E., additional, Zamorani, G., additional, Gilli, R., additional, La Franca, F., additional, Lanzuisi, G., additional, Lutz, D., additional, Santini, P., additional, Scoville, N. Z., additional, Vignali, C., additional, Vito, F., additional, Rabien, S., additional, Busoni, L., additional, and Bonaglia, M., additional

Published
2018
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39. Dust and gas in star-forming galaxies at z ~ 3

Author

Magdis, G. E., primary, Rigopoulou, D., additional, Daddi, E., additional, Bethermin, M., additional, Feruglio, C., additional, Sargent, M., additional, Dannerbauer, H., additional, Dickinson, M., additional, Elbaz, D., additional, Gomez Guijarro, C., additional, Huang, J.-S., additional, Toft, S., additional, and Valentino, F., additional

Published
2017
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40. Molecular gas, dust, and star formation in galaxies

Author

Orellana, G., primary, Nagar, N. M., additional, Elbaz, D., additional, Calderón-Castillo, P., additional, Leiton, R., additional, Ibar, E., additional, Magnelli, B., additional, Daddi, E., additional, Messias, H., additional, Cerulo, P., additional, and Slater, R., additional

Published
2017
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41. AGN-host connection at 0.5 < z < 2.5: A rapid evolution of AGN fraction in red galaxies during the last 10 Gyr

Author

Wang, Tao, primary, Elbaz, D., additional, Alexander, D. M., additional, Xue, Y. Q., additional, Gabor, J. M., additional, Juneau, S., additional, Schreiber, C., additional, Zheng, X.-Z., additional, Wuyts, S., additional, Shi, Y., additional, Daddi, E., additional, Shu, X.-W., additional, Fang, G.-W., additional, Huang, J.-S., additional, Luo, B., additional, and Gu, Q.-S., additional

Published
2017
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42. In and out star formation inz ~ 1.5 quiescent galaxies from rest-frame UV spectroscopy and the far-infrared

Author

Gobat, R., primary, Daddi, E., additional, Strazzullo, V., additional, Garilli, B., additional, Mignoli, M., additional, Ma, Z., additional, Jin, S., additional, Maraston, C., additional, Magdis, G., additional, Béthermin, M., additional, Cappellari, M., additional, Carollo, M., additional, Cimatti, A., additional, Feruglio, C., additional, Moresco, M., additional, Onodera, M., additional, Pozzetti, L., additional, Renzini, A., additional, Sargent, M., additional, Valentino, F., additional, and Zanella, A., additional

Published
2017
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43. Characterizing elusive, faint dusty star-forming galaxies: a lensed, optically undetected ALMA galaxy atz ~ 3.3

Author

Santini, P., primary, Castellano, M., additional, Fontana, A., additional, Merlin, E., additional, Maiolino, R., additional, Mason, C., additional, Mignano, A., additional, Pilo, S., additional, Amorin, R., additional, Berta, S., additional, Bourne, N., additional, Calura, F., additional, Daddi, E., additional, Elbaz, D., additional, Grazian, A., additional, Magliocchetti, M., additional, Michałowski, M. J., additional, Pentericci, L., additional, Pozzi, F., additional, Rodighiero, G., additional, Schreiber, C., additional, and Valiante, R., additional

Published
2016
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44. Deciphering an evolutionary sequence of merger stages in infrared-luminous starburst galaxies at z ∼ 0.7.

Author

Calabrò, A., Daddi, E., Puglisi, A., Oliva, E., Gobat, R., Cassata, P., Amorín, R., Arimoto, N., Boquien, M., Carraro, R., Delvecchio, I., Ibar, E., Jin, S., Juneau, S., Liu, D., Onodera, M., Mannucci, F., Méndez-Hernández, H., Rodighiero, G., and Valentino, F.

Subjects
*STARBURSTS, *ELLIPTICAL galaxies, *GRAVITATIONAL potential, *STELLAR populations, *GALAXIES, *POTENTIAL well
Abstract

Based on optical and near-IR Magellan FIRE spectra of 25 starburst galaxies at 0.5 <  z <  0.9, a recent publication showed that their attenuation properties can be explained by a single-parameter sequence of total obscurations ranging from AV = 2 to AV = 30 toward the starburst core centers in a mixed stars and dust configuration. We investigate here the origin of this sequence for the same sample. We show that total attenuations anticorrelate with the starburst sizes in radio (3 GHz) with a significance larger than 5σ and a scatter of 0.26 dex. More obscured and compact starbursts also show enhanced N2 (=[NII]/Hα) ratios and larger line velocity widths that we attribute to an increasing shock contribution toward later merger phases, driven by deeper gravitational potential wells at the coalescence. Additionally, the attenuation is also linked to the equivalent width (EW) of hydrogen recombination lines, which is sensitive to the luminosity weighted age of the relatively unobscured stellar populations. Overall, the correlations among AV, tot, radio size, line width, N2 and EW of Balmer and Paschen lines converge toward suggesting an evolutionary sequence of merger stages: all of these quantities are likely to be good time-tracers of the merger phenomenon, and their large spanned range appears to be characteristic of the different merger phases. Half of our sample at higher obscurations have radio sizes approximately 3 times smaller than early type galaxies at the same redshift, suggesting that, in analogy with local ultraluminous infrared galaxies (ULIRGs), these cores cannot be directly forming elliptical galaxies. Finally, we detect mid-IR AGN torus for half of our sample and additional X-ray emission for 6 starbursts; intriguingly, the latter have systematically more compact sizes, suggestive of emerging AGNs toward later merger stages, possibly precursors of a later QSO phase. [ABSTRACT FROM AUTHOR]

Published
2019
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46. Dust attenuation inz~ 1 galaxies fromHerscheland 3D-HST Hαmeasurements

Author

Puglisi, A., primary, Rodighiero, G., additional, Franceschini, A., additional, Talia, M., additional, Cimatti, A., additional, Baronchelli, I., additional, Daddi, E., additional, Renzini, A., additional, Schawinski, K., additional, Mancini, C., additional, Silverman, J., additional, Gruppioni, C., additional, Lutz, D., additional, Berta, S., additional, and Oliver, S. J., additional

Published
2016
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47. Modeling CO emission from hydrodynamic simulations of nearby spirals, starbursting mergers, and high-redshift galaxies

Author

Bournaud, F, Daddi, E, Weiß, A, Renaud, F, Mastropietro, C, Teyssier, R, Bournaud, F, Daddi, E, Weiß, A, Renaud, F, Mastropietro, C, and Teyssier, R

Abstract

We model the intensity of emission lines from the CO molecule, based on hydrodynamic simulations of spirals, mergers, and high-redshift galaxies with very high resolutions (3 pc and 103 M⊙) and detailed models for the phase-space structure of the interstellar gas including shock heating, stellar feedback processes, and galactic winds. The simulations are analyzed with a large velocity gradient (LVG) model to compute the local emission in various molecular lines in each resolution element, radiation transfer, opacity effect, and the intensity emerging from galaxies to generate synthetic spectra for various transitions of the CO molecule. This model reproduces the known properties of CO spectra and CO-to-H2 conversion factors in nearby spirals and starbursting major mergers. The high excitation of CO lines in mergers is dominated by an excess of high-density gas, and the high turbulent velocities and compression that create this dense gas excess result in broad linewidths and low CO intensity-to-H2 mass ratios. When applied to high-redshift gas-rich disks galaxies, the same model predicts that their CO-to-H2 conversion factor is almost as high as in nearby spirals, and much higher than in starbursting mergers. High-redshift disk galaxies contain giant star-forming clumps that host a high-excitation component associated to gas warmed by the spatially concentrated stellar feedback sources, although CO(1-0) to CO(3-2) emission is dominated overall by low-excitation gas around the densest clumps. These results generally highlight a strong dependence of CO excitation and the CO-to-H2 conversion factor on galaxy type, even at similar star formation rates or densities. The underlying processes are driven by the interstellar medium structure and turbulence and its response to stellar feedback, which depend on global galaxy structure and in turn affect the CO emission properties.

Published
2015

49. Satellite content and quenching of star formation in galaxy groups atz~ 1.8

Author

Gobat, R., primary, Daddi, E., additional, Béthermin, M., additional, Pannella, M., additional, Finoguenov, A., additional, Gozaliasl, G., additional, Le Floc’h, E., additional, Schreiber, C., additional, Strazzullo, V., additional, Sargent, M., additional, Wang, T., additional, Hwang, H. S., additional, Valentino, F., additional, Cappelluti, N., additional, Li, Y., additional, and Hasinger, G., additional

Published
2015
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50. Evidence for feedback in action from the molecular gas content in thez~ 1.6 outflowing QSO XID2028

Author

Brusa, M., primary, Feruglio, C., additional, Cresci, G., additional, Mainieri, V., additional, Sargent, M. T., additional, Perna, M., additional, Santini, P., additional, Vito, F., additional, Marconi, A., additional, Merloni, A., additional, Lutz, D., additional, Piconcelli, E., additional, Lanzuisi, G., additional, Maiolino, R., additional, Rosario, D., additional, Daddi, E., additional, Bongiorno, A., additional, Fiore, F., additional, and Lusso, E., additional

Published
2015
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