[{"date_published":"2020-03-11T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/2002.05731","open_access":"1"}],"publication":"Astronomy & Astrophysics","month":"03","article_number":"A82","oa_version":"Published Version","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"external_id":{"arxiv":["2002.05731"]},"date_updated":"2022-07-19T09:36:58Z","year":"2020","citation":{"ista":"Leclercq F, Bacon R, Verhamme A, Garel T, Blaizot J, Brinchmann J, Cantalupo S, Claeyssens A, Conseil S, Contini T, Hashimoto T, Herenz EC, Kusakabe H, Marino RA, Maseda M, Matthee JJ, Mitchell P, Pezzulli G, Richard J, Schmidt KB, Wisotzki L. 2020. The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z &#62; 3. Astronomy &#38; Astrophysics. 635, A82.","short":"F. Leclercq, R. Bacon, A. Verhamme, T. Garel, J. Blaizot, J. Brinchmann, S. Cantalupo, A. Claeyssens, S. Conseil, T. Contini, T. Hashimoto, E.C. Herenz, H. Kusakabe, R.A. Marino, M. Maseda, J.J. Matthee, P. Mitchell, G. Pezzulli, J. Richard, K.B. Schmidt, L. Wisotzki, Astronomy &#38; Astrophysics 635 (2020).","mla":"Leclercq, Floriane, et al. “The MUSE Hubble Ultra Deep Field Survey: XIII. Spatially Resolved Spectral Properties of Lyman α Haloes around Star-Forming Galaxies at z &#62; 3.” <i>Astronomy &#38; Astrophysics</i>, vol. 635, A82, EDP Sciences, 2020, doi:<a href=\"https://doi.org/10.1051/0004-6361/201937339\">10.1051/0004-6361/201937339</a>.","ieee":"F. Leclercq <i>et al.</i>, “The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z &#62; 3,” <i>Astronomy &#38; Astrophysics</i>, vol. 635. EDP Sciences, 2020.","chicago":"Leclercq, Floriane, Roland Bacon, Anne Verhamme, Thibault Garel, Jérémy Blaizot, Jarle Brinchmann, Sebastiano Cantalupo, et al. “The MUSE Hubble Ultra Deep Field Survey: XIII. Spatially Resolved Spectral Properties of Lyman α Haloes around Star-Forming Galaxies at z &#62; 3.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2020. <a href=\"https://doi.org/10.1051/0004-6361/201937339\">https://doi.org/10.1051/0004-6361/201937339</a>.","apa":"Leclercq, F., Bacon, R., Verhamme, A., Garel, T., Blaizot, J., Brinchmann, J., … Wisotzki, L. (2020). The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z &#62; 3. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201937339\">https://doi.org/10.1051/0004-6361/201937339</a>","ama":"Leclercq F, Bacon R, Verhamme A, et al. The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z &#62; 3. <i>Astronomy &#38; Astrophysics</i>. 2020;635. doi:<a href=\"https://doi.org/10.1051/0004-6361/201937339\">10.1051/0004-6361/201937339</a>"},"abstract":[{"lang":"eng","text":"We present spatially resolved maps of six individually-detected Lyman α haloes (LAHs) as well as a first statistical analysis of the Lyman α (Lyα) spectral signature in the circum-galactic medium of high-redshift star-forming galaxies (−17.5 >  MUV >  −21.5) using the Multi-Unit Spectroscopic Explorer. Our resolved spectroscopic analysis of the LAHs reveals significant intrahalo variations of the Lyα line profile. Using a three-dimensional two-component model for the Lyα emission, we measured the full width at half maximum (FWHM), the peak velocity shift, and the asymmetry of the Lyα line in the core and in the halo of 19 galaxies. We find that the Lyα line shape is statistically different in the halo compared to the core (in terms of width, peak wavelength, and asymmetry) for ≈40% of our galaxies. Similarly to object-by-object based studies and a recent resolved study using lensing, we find a correlation between the peak velocity shift and the width of the Lyα line both at the interstellar and circum-galactic scales. This trend has been predicted by radiative transfer simulations of galactic winds as a result of resonant scattering in outflows. While there is a lack of correlation between the spectral properties and the spatial scale lengths of our LAHs, we find a correlation between the width of the line in the LAH and the halo flux fraction. Interestingly, UV bright galaxies (MUV <  −20) show broader, more redshifted, and less asymmetric Lyα lines in their haloes. The most significant correlation found is for the FWHM of the line and the UV continuum slope of the galaxy, suggesting that the redder galaxies have broader Lyα lines. The generally broad and red line shapes found in the halo component suggest that the Lyα haloes are powered either by scattering processes through an outflowing medium, fluorescent emission from outflowing cold clumps of gas, or a mix of both. Considering the large diversity of the Lyα line profiles observed in our sample and the lack of strong correlation, the interpretation of our results is still broadly open and underlines the need for realistic spatially resolved models of the LAHs."}],"arxiv":1,"doi":"10.1051/0004-6361/201937339","day":"11","extern":"1","volume":635,"acknowledgement":"F.L., R.B., and S.C. acknowledge support from the ERC advanced grant 339659-MUSICOS. F.L., T.G., H.K., and A.V. acknowledge support from the ERC starting grant ERC-757258-TRIPLE. A.C. and J.R. acknowledge support from the ERC starting grant 336736-CALENDS. J.B. acknowledges support by FCT/MCTES through national funds (PID-DAC) by grant UID/FIS/04434/2019 and through Investigador FCT Contract No.IF/01654/2014/CP1215/CT0003. T.H. was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan.","author":[{"first_name":"Floriane","last_name":"Leclercq","full_name":"Leclercq, Floriane"},{"full_name":"Bacon, Roland","first_name":"Roland","last_name":"Bacon"},{"last_name":"Verhamme","first_name":"Anne","full_name":"Verhamme, Anne"},{"first_name":"Thibault","last_name":"Garel","full_name":"Garel, Thibault"},{"full_name":"Blaizot, Jérémy","first_name":"Jérémy","last_name":"Blaizot"},{"last_name":"Brinchmann","first_name":"Jarle","full_name":"Brinchmann, Jarle"},{"full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano","last_name":"Cantalupo"},{"last_name":"Claeyssens","first_name":"Adélaïde","full_name":"Claeyssens, Adélaïde"},{"full_name":"Conseil, Simon","last_name":"Conseil","first_name":"Simon"},{"last_name":"Contini","first_name":"Thierry","full_name":"Contini, Thierry"},{"first_name":"Takuya","last_name":"Hashimoto","full_name":"Hashimoto, Takuya"},{"full_name":"Herenz, Edmund Christian","first_name":"Edmund Christian","last_name":"Herenz"},{"last_name":"Kusakabe","first_name":"Haruka","full_name":"Kusakabe, Haruka"},{"full_name":"Marino, Raffaella Anna","last_name":"Marino","first_name":"Raffaella Anna"},{"full_name":"Maseda, Michael","first_name":"Michael","last_name":"Maseda"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"first_name":"Peter","last_name":"Mitchell","full_name":"Mitchell, Peter"},{"last_name":"Pezzulli","first_name":"Gabriele","full_name":"Pezzulli, Gabriele"},{"full_name":"Richard, Johan","last_name":"Richard","first_name":"Johan"},{"full_name":"Schmidt, Kasper Borello","last_name":"Schmidt","first_name":"Kasper Borello"},{"last_name":"Wisotzki","first_name":"Lutz","full_name":"Wisotzki, Lutz"}],"_id":"11504","scopus_import":"1","title":"The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3","intvolume":"       635","publication_status":"published","date_created":"2022-07-06T09:56:20Z","article_processing_charge":"No","quality_controlled":"1","article_type":"original","publisher":"EDP Sciences"},{"oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"type":"journal_article","date_published":"2019-03-01T00:00:00Z","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1805.05956","open_access":"1"}],"month":"03","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics : galaxies: evolution","galaxies: formation","galaxies: star formation","cosmology: theory"],"language":[{"iso":"eng"}],"abstract":[{"lang":"eng","text":"Observations have revealed that the star formation rate (SFR) and stellar mass (Mstar) of star-forming galaxies follow a tight relation known as the galaxy main sequence. However, what physical information is encoded in this relation is under debate. Here, we use the EAGLE cosmological hydrodynamical simulation to study the mass dependence, evolution, and origin of scatter in the SFR–Mstar relation. At z = 0, we find that the scatter decreases slightly with stellar mass from 0.35 dex at Mstar ≈ 109 M⊙ to 0.30 dex at Mstar ≳ 1010.5 M⊙. The scatter decreases from z = 0 to z = 5 by 0.05 dex at Mstar ≳ 1010 M⊙ and by 0.15 dex for lower masses. We show that the scatter at z = 0.1 originates from a combination of fluctuations on short time-scales (ranging from 0.2–2 Gyr) that are presumably associated with self-regulation from cooling, star formation, and outflows, but is dominated by long time-scale (∼10 Gyr) variations related to differences in halo formation times. Shorter time-scale fluctuations are relatively more important for lower mass galaxies. At high masses, differences in black hole formation efficiency cause additional scatter, but also diminish the scatter caused by different halo formation times. While individual galaxies cross the main sequence multiple times during their evolution, they fluctuate around tracks associated with their halo properties, i.e. galaxies above/below the main sequence at z = 0.1 tend to have been above/below the main sequence for ≫1 Gyr."}],"day":"01","doi":"10.1093/mnras/stz030","arxiv":1,"external_id":{"arxiv":["1805.05956"]},"year":"2019","citation":{"apa":"Matthee, J. J., &#38; Schaye, J. (2019). The origin of scatter in the star formation rate–stellar mass relation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz030\">https://doi.org/10.1093/mnras/stz030</a>","ama":"Matthee JJ, Schaye J. The origin of scatter in the star formation rate–stellar mass relation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;484(1):915-932. doi:<a href=\"https://doi.org/10.1093/mnras/stz030\">10.1093/mnras/stz030</a>","ieee":"J. J. Matthee and J. Schaye, “The origin of scatter in the star formation rate–stellar mass relation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 484, no. 1. Oxford University Press, pp. 915–932, 2019.","chicago":"Matthee, Jorryt J, and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/stz030\">https://doi.org/10.1093/mnras/stz030</a>.","mla":"Matthee, Jorryt J., and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 484, no. 1, Oxford University Press, 2019, pp. 915–32, doi:<a href=\"https://doi.org/10.1093/mnras/stz030\">10.1093/mnras/stz030</a>.","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society 484 (2019) 915–932.","ista":"Matthee JJ, Schaye J. 2019. The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. 484(1), 915–932."},"date_updated":"2022-08-19T06:42:43Z","extern":"1","acknowledgement":"JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Camila Correa for help analysing snipshot merger trees. We thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann, Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and ideas. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT analysis tool (Taylor 2013).","volume":484,"intvolume":"       484","title":"The origin of scatter in the star formation rate–stellar mass relation","article_processing_charge":"No","date_created":"2022-07-08T07:48:31Z","publication_status":"published","issue":"1","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"}],"scopus_import":"1","_id":"11540","article_type":"original","publisher":"Oxford University Press","quality_controlled":"1","page":"915-932"},{"day":"01","doi":"10.1093/mnras/stx1569","arxiv":1,"abstract":[{"lang":"eng","text":"We present a sample of ∼1000 emission-line galaxies at z = 0.4–4.7 from the ∼0.7deg2 High-z Emission-Line Survey in the Boötes field identified with a suite of six narrow-band filters at ≈0.4–2.1 μm. These galaxies have been selected on their Ly α (73), [O II] (285), H β/[O III] (387) or H α (362) emission line, and have been classified with optical to near-infrared colours. A subsample of 98 sources have reliable redshifts from multiple narrow-band (e.g. [O II]–H α) detections and/or spectroscopy. In this survey paper, we present the observations, selection and catalogues of emitters. We measure number densities of Ly α, [O II], H β/[O III] and H α and confirm strong luminosity evolution in star-forming galaxies from z ∼ 0.4 to ∼5, in agreement with previous results. To demonstrate the usefulness of dual-line emitters, we use the sample of dual [O II]–H α emitters to measure the observed [O II]/H α ratio at z = 1.47. The observed [O II]/H α ratio increases significantly from 0.40 ± 0.01 at z = 0.1 to 0.52 ± 0.05 at z = 1.47, which we attribute to either decreasing dust attenuation with redshift, or due to a bias in the (typically) fibre measurements in the local Universe that only measure the central kpc regions. At the bright end, we find that both the H α and Ly α number densities at z ≈ 2.2 deviate significantly from a Schechter form, following a power law. We show that this is driven entirely by an increasing X-ray/active galactic nucleus fraction with line luminosity, which reaches ≈100 per cent at line luminosities L ≳ 3 × 1044 erg s−1."}],"citation":{"ama":"Matthee JJ, Sobral D, Best P, et al. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(1):629-649. doi:<a href=\"https://doi.org/10.1093/mnras/stx1569\">10.1093/mnras/stx1569</a>","apa":"Matthee, J. J., Sobral, D., Best, P., Smail, I., Bian, F., Darvish, B., … Fan, X. (2017). Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1569\">https://doi.org/10.1093/mnras/stx1569</a>","chicago":"Matthee, Jorryt J, David Sobral, Philip Best, Ian Smail, Fuyan Bian, Behnam Darvish, Huub Röttgering, and Xiaohui Fan. “Boötes-HiZELS: An Optical to near-Infrared Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1569\">https://doi.org/10.1093/mnras/stx1569</a>.","ieee":"J. J. Matthee <i>et al.</i>, “Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 1. Oxford University Press, pp. 629–649, 2017.","short":"J.J. Matthee, D. Sobral, P. Best, I. Smail, F. Bian, B. Darvish, H. Röttgering, X. Fan, Monthly Notices of the Royal Astronomical Society 471 (2017) 629–649.","mla":"Matthee, Jorryt J., et al. “Boötes-HiZELS: An Optical to near-Infrared Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 1, Oxford University Press, 2017, pp. 629–49, doi:<a href=\"https://doi.org/10.1093/mnras/stx1569\">10.1093/mnras/stx1569</a>.","ista":"Matthee JJ, Sobral D, Best P, Smail I, Bian F, Darvish B, Röttgering H, Fan X. 2017. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. Monthly Notices of the Royal Astronomical Society. 471(1), 629–649."},"year":"2017","date_updated":"2022-08-19T07:15:14Z","external_id":{"arxiv":["1702.04721"]},"volume":471,"extern":"1","date_created":"2022-07-12T11:01:35Z","article_processing_charge":"No","publication_status":"published","intvolume":"       471","title":"Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7","scopus_import":"1","_id":"11561","issue":"1","author":[{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"first_name":"Philip","last_name":"Best","full_name":"Best, Philip"},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"full_name":"Bian, Fuyan","first_name":"Fuyan","last_name":"Bian"},{"full_name":"Darvish, Behnam","first_name":"Behnam","last_name":"Darvish"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"full_name":"Fan, Xiaohui","last_name":"Fan","first_name":"Xiaohui"}],"publisher":"Oxford University Press","article_type":"original","quality_controlled":"1","page":"629-649","publication_identifier":{"issn":["0035-8711","1365-2966"]},"oa":1,"type":"journal_article","date_published":"2017-10-01T00:00:00Z","main_file_link":[{"url":"https://arxiv.org/abs/1702.04721","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","oa_version":"Preprint","month":"10","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics galaxies","active","galaxies","evolution","galaxies","high-redshift","galaxies","luminosity function","mass function","galaxies: star formation"],"language":[{"iso":"eng"}]}]