MIDIS: Strong (Hβ+[O iii]) and Hα Emitters at Redshift z ≃ 7–8 Unveiled with JWST NIRCam and MIRI Imaging in the Hubble eXtreme Deep Field

Rinaldi, Pierluigi; Caputi, K.; Costantin, Luca; Gillman, Steven; Iani, Edoardo; Pérez‐González, Pablo G.; Östlin, Göran; Colina, L.; Greve, T. R.; Noorgard-Nielsen, H. U.; S., Wright, G.; Alonso‐Herrero, A.; Álvarez-Márquez, J.; Eckart, A.; Marín, Macarena García; Hjorth, J.; Ilbert, O.; Kendrew, Sarah; Labiano, Á.; Fèvre, O. Le; Pye, J. P.; T., Tikkanen,; Walter, Fabian; Werf, P. P. van der; Ward, M. J.; Annunziatella, Marianna; Azzollini, R.; Bik, Arjan; Boogaard, Leindert; Gómez, A.; Jermann, Iris; Langeroodi, Danial; Melinder, Jens; Meyer, Romain A.; Moutard, T.; Peißker, F.; M., Topinka,; Dishoeck, Ewine van; Guêdel, M.; Henning, Thomas; Lagage, Pierre-Olivier; Ray, T. P.; Vandenbussche, B.; Waelkens, C.; Navarro-Carrera, Rafael; Kokorev, Vasily

doi:10.3847/1538-4357/acdc27

Cited by 22 publications

(52 citation statements)

References 95 publications

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“…Deep photometric investigations have also confirmed the monotonic increase in the merger rate until z = 6 (Duncan et al 2019). We hypothesize that the increased merger rate might be responsible for the overabundance of EELGs detected with JWST at z > 6 (Cameron et al 2023;Endsley et al 2023;Rinaldi et al 2023;Tang et al 2023). Thus, properly accounting for mergers would be important while estimating physical properties of gas and stars, in particular their kinematics and morphology in the early Universe.…”

Section: Discussionmentioning

confidence: 79%

“…In the past decade, deep photometric surveys with Spitzer and Hubble Space Telescope (HST) revealed more than two orders increase in the [O III] 5007+Hβ equivalent width (EW) of galaxies between z = 0 and 6 (Labbé et al 2013;Roberts-Borsani et al 2016;Barro et al 2019;Mainali et al 2019;Endsley et al 2020;Gupta et al 2022). Direct observations with the James Webb Space Telescope (JWST) in the past year have confirmed that 80% of galaxies have [O III] 5007+Hβ EW >800 Å; almost 3 times the EW of a typical star-forming galaxy at z ∼ 2 (Cameron et al 2023;Endsley et al 2023;Rinaldi et al 2023;Tang et al 2023). Thus, understanding the physical origin of extreme emission lines is becoming increasingly important to understand the early galaxy evolution.…”

Section: Introductionmentioning

confidence: 99%

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MOSEL Survey: JWST Reveals Major Mergers/strong Interactions Drive the Extreme Emission Lines in the Early Universe

Gupta,

Jaiswar,

Rodriguez-Gomez

et al. 2023

ApJL

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Extreme emission line galaxies (EELGs), where nebular emissions contribute 30%–40% of the flux in certain photometric bands, are ubiquitous in the early Universe (z > 6). We utilize deep NIRCam imaging from the JWST Advanced Deep Extragalactic Survey (JADES) to investigate the properties of companion galaxies (projected distance <40 kpc, ∣dv∣ < 10,000 km s−1) around EELGs at z ∼ 3. Tests with TNG100 simulation reveal that nearly all galaxies at z = 3 will merge with at least one companion galaxy selected using similar parameters by z = 0. The median mass ratio of the most massive companion and the total mass ratio of all companions around EELGs is more than 10 times higher the control sample. Even after comparing with a stellar mass and stellar mass plus specific star formation rate (SFR)-matched control sample, EELGs have 3 to 5 times higher mass ratios than the brightest companion and total mass ratio of all companions. Our measurements suggest that EELGs are more likely to be experiencing strong interactions or undergoing major mergers irrespective of their stellar mass or specific SFRs. We suspect that gas cooling induced by strong interactions and/or major mergers could be triggering the extreme emission lines, and the increased merger rate might be responsible for the overabundance of EELGs at z > 6.

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Section: Discussionmentioning

confidence: 79%

Section: Introductionmentioning

confidence: 99%

MOSEL Survey: JWST Reveals Major Mergers/strong Interactions Drive the Extreme Emission Lines in the Early Universe

Gupta,

Jaiswar,

Rodriguez-Gomez

et al. 2023

ApJL

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“…The left and right panels of Figure 4 illustrate several important points about our sample of EELGs. First, a visual inspection of the left panel of Figure 4 shows that our sample reproduces the known anticorrelation between rest-frame EW(Hα) and stellar mass (e.g., Onodera et al 2020;Matthee et al 2023;Rinaldi et al 2023). However, there does not appear to be any correlation .…”

Section: Dependence Of Equivalent Widths On Physical Properties and R...mentioning

confidence: 75%

“…Early JWST studies of EELGs have already begun to yield interesting results. These include the identification of very high EW systems (EW >1000 Å for [O III] + Hβ and Hα) up to z ∼ 9 and confirmation that EELGs are common in the high-z Universe (e.g., Kashino et al 2023;Laporte et al 2023;Matthee et al 2023;Rinaldi et al 2023;Williams et al 2023). Other work has shown that the hydrogen-ionizing photonproduction efficiencies (ξ ion ) of high-z EELGs are generally high, as expected if these objects are responsible for reionization (e.g., Asada et al 2023;Sun et al 2023).…”

Section: Introductionmentioning

confidence: 77%

“…Extreme emission-line galaxies (EELGs) have become a major field of study in recent years, with many searches targeting EELGs in the local Universe up to high redshifts (e.g., local Universe, Cardamone et al 2009;Henry et al 2018;Liu et al 2022;intermediate z, van der Wel et al 2011;Maseda et al 2014Maseda et al , 2018Tang et al 2019;Onodera et al 2020;Tran et al 2020;Rosenwasser et al 2022;Boyett et al 2022;Gupta et al 2023;high z, Stark et al 2013;Smit et al 2014;Roberts-Borsani et al 2016;Stark et al 2017;Endsley et al 2021;Kashino et al 2023;Matthee et al 2023;Asada et al 2023;Laporte et al 2023;Williams et al 2023;Rinaldi et al 2023;Ning et al 2023). Regardless of their redshift, EELGs are characterized by high equivalent-width (EW) UV-optical emission lines driven by elevated star formation, generally found in low-mass, metal-poor galaxies with little dust.…”

Section: Introductionmentioning

confidence: 99%

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Spectroscopy from Photometry: A Population of Extreme Emission Line Galaxies at 1.7 ≲ z ≲ 6.7 Selected with JWST Medium Band Filters

Withers,

Muzzin,

Ravindranath

et al. 2023

ApJL

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We use JWST/NIRCam medium band photometry in a single pointing of the Canadian NIRISS Unbiased Cluster Survey to identify 118 extreme emission-line galaxies (EELGs) over 1.7 ≲ z ≲ 6.7, selected using a set of color cuts that target galaxies with extreme [O iii] + Hβ and Hα emission. We show that our medium band color selections are able to select galaxies based on emission-line EW, which is advantageous to more commonly used selections since it does not require strong continuum emission, and can select galaxies with faint or red continuum fluxes. The median EWs of our sample is EW(Hα) = 893 Å and EW ([O III] + Hβ) = 1255 Å and includes some objects with EW ([O III] + Hβ) ∼ 3000 Å. These systems are mostly compact with low stellar mass (median log ( M ⋆ / M ⊙ ) = 8.03 ), low metallicity (median Z = 0.14 Z ⊙), little dust (median A V = 0.18 mag), and high SSFR (median SSFR = 1.18 × 10−8 yr−1). Additionally, galaxies in our sample show increasing EW(Hα) and EW([O iii] + Hβ) with redshift, an anticorrelation of EW(Hα) with stellar mass, and no correlation between EW([O iii] + Hβ) and stellar mass. Finally, we present NIRSpec spectroscopy of 15 of the EELGs in our sample. These spectra confirm the redshifts and EWs of the EELGs calculated from the medium bands, which demonstrates the accuracy and efficiency of our color selections. Overall, we show that there are significant advantages to using medium band photometry to identify and study EELGs at a wide range of redshifts.

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An extremely metal-poor star complex in the reionization era: Approaching Population III stars with JWST

Vanzella,

Loiacono,

Bergamini

et al. 2023

A&A

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We present JWST/Near Infrared Spectrograph (NIRSpec) integral field spectroscopy (IFS) of a lensed Population III candidate stellar complex (dubbed Lensed And Pristine 1, LAP1), with a lensing-corrected stellar mass of ≲104 M⊙ and an absolute luminosity of MUV > −11.2 (mUV > 35.6), confirmed at redshift 6.639 ± 0.004. The system is strongly amplified (μ ≳ 100) by straddling a critical line of the Hubble Frontier Field galaxy cluster MACS J0416. Although the stellar continuum is currently not detected in the Hubble and JWST/Near Infrared Camera (NIRCam) and Near Infrared Imager and Slitless Spectrograph (NIRISS) imaging, arclet-like shapes of Lyman and Balmer lines, Lyα, Hγ, Hβ and Hα are detected with NIRSpec IFS with signal-to-noise ratios (S/N) of approximately 5 − 13 and large equivalent widths (> 300 − 2000 Å), along with a remarkably weak [O III]λλ4959, 5007 at S/N ≃ 4. LAP1 shows a large ionizing photon production efficiency, log(ξion[erg Hz−1]) > 26. From the metallicity indexes R23 = ([O III] + [O II])/Hβ ≲ 0.74 and R3 = ([O III]/Hβ) = 0.55 ± 0.14, we derive an oxygen abundance of 12 + log(O/H)≲6.3. Intriguingly, the Hα emission is also measured in mirrored subcomponents where no [O III] is detected, providing even more stringent upper limits on the metallicity if in situ star formation is ongoing in this region (12 + log(O/H) < 6). The formal stellar mass limit of the subcomponents would correspond to ∼103 M⊙ or MUV fainter than −10. Alternatively, this metal-free, pure line-emitting region could be the first case of a fluorescing H I gas region induced by transverse escaping ionizing radiation from a nearby star complex. The presence of large equivalent-width hydrogen lines and the deficiency of metal lines in such a small region make LAP1 the most metal-poor star-forming region currently known in the reionization era and a promising site that may host isolated, pristine stars.

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MIDIS: Strong (Hβ+[O iii]) and Hα Emitters at Redshift z ≃ 7–8 Unveiled with JWST NIRCam and MIRI Imaging in the Hubble eXtreme Deep Field

Cited by 22 publications

References 95 publications

MOSEL Survey: JWST Reveals Major Mergers/strong Interactions Drive the Extreme Emission Lines in the Early Universe

MOSEL Survey: JWST Reveals Major Mergers/strong Interactions Drive the Extreme Emission Lines in the Early Universe

Spectroscopy from Photometry: A Population of Extreme Emission Line Galaxies at 1.7 ≲ z ≲ 6.7 Selected with JWST Medium Band Filters

An extremely metal-poor star complex in the reionization era: Approaching Population III stars with JWST

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