RIOJA. Complex Dusty Starbursts in a Major Merger B14-65666 at z=7.15
Fuente:
arXiv
Enregistré dans:
| Auteurs principaux: | , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Format: | Preprint |
| Publié: |
2024
|
| Sujets: | |
| Accès en ligne: | |
| Tags: |
Ajouter un tag
Pas de tags, Soyez le premier à ajouter un tag!
|
| _version_ | 1866909484589252608 |
|---|---|
| author | Sugahara, Yuma Álvarez-Márquez, Javier Hashimoto, Takuya Colina, Luis Inoue, Akio K. Costantin, Luca Fudamoto, Yoshinobu Mawatari, Ken Ren, Yi W. Arribas, Santiago Bakx, Tom J. L. C. Blanco-Prieto, Carmen Ceverino, Daniel Gómez, Alejandro Crespo Hagimoto, Masato Hashigaya, Takeshi Marques-Chaves, Rui Matsuo, Hiroshi Nakazato, Yurina Pereira-Santaella, Miguel Tamura, Yoichi Usui, Mitsutaka Yoshida, Naoki |
| author_facet | Sugahara, Yuma Álvarez-Márquez, Javier Hashimoto, Takuya Colina, Luis Inoue, Akio K. Costantin, Luca Fudamoto, Yoshinobu Mawatari, Ken Ren, Yi W. Arribas, Santiago Bakx, Tom J. L. C. Blanco-Prieto, Carmen Ceverino, Daniel Gómez, Alejandro Crespo Hagimoto, Masato Hashigaya, Takeshi Marques-Chaves, Rui Matsuo, Hiroshi Nakazato, Yurina Pereira-Santaella, Miguel Tamura, Yoichi Usui, Mitsutaka Yoshida, Naoki |
| contents | We present JWST NIRCam imaging of B14-65666 ("Big Three Dragons"), a bright Lyman-break galaxy system ($M_\text{UV}=-22.5$ mag) at $z=7.15$. The high angular resolution of NIRCam reveals the complex morphology of two galaxy components: galaxy E has a compact core (E-core), surrounded by diffuse, extended, rest-frame optical emission, which is likely to be tidal tails; and galaxy W has a clumpy and elongated morphology with a blue UV slope ($β_\text{UV}=-2.2\pm0.1$). The flux excess, F356W$-$F444W, peaks at the E-core ($1.05^{+0.08}_{-0.09}$ mag), tracing the presence of strong [OIII] 4960,5008 Å emission. ALMA archival data show that the bluer galaxy W is brighter in dust continua than the redder galaxy E, while the tails are bright in [OIII] 88 $\mathrm{μm}$. The UV/optical and sub-mm SED fitting confirms that B14-65666 is a major merger in a starburst phase as derived from the stellar mass ratio (3:1 to 2:1) and the star-formation rate, $\simeq1$ dex higher than the star-formation main sequence at the same redshift. The galaxy E is a dusty ($A_\text{V}=1.2\pm0.1$ mag) starburst with a possible high dust temperature ($\ge63$-$68$ K). The galaxy W would have a low dust temperature ($\le27$-$33$ K) or patchy stellar-and-dust geometry, as suggested from the infrared excess (IRX) and $β_\text{UV}$ diagram. The high optical-to-FIR [OIII] line ratio of the E-core shows its lower gas-phase metallicity ($\simeq0.2$-$0.4$ Z$_{\odot}$) than the galaxy W. These results agree with a scenario where major mergers disturb morphology and induce nuclear dusty starbursts triggered by less-enriched inflows. B14-65666 shows a picture of complex stellar buildup processes during major mergers in the epoch of reionization. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2403_17133 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | RIOJA. Complex Dusty Starbursts in a Major Merger B14-65666 at z=7.15 Sugahara, Yuma Álvarez-Márquez, Javier Hashimoto, Takuya Colina, Luis Inoue, Akio K. Costantin, Luca Fudamoto, Yoshinobu Mawatari, Ken Ren, Yi W. Arribas, Santiago Bakx, Tom J. L. C. Blanco-Prieto, Carmen Ceverino, Daniel Gómez, Alejandro Crespo Hagimoto, Masato Hashigaya, Takeshi Marques-Chaves, Rui Matsuo, Hiroshi Nakazato, Yurina Pereira-Santaella, Miguel Tamura, Yoichi Usui, Mitsutaka Yoshida, Naoki Astrophysics of Galaxies We present JWST NIRCam imaging of B14-65666 ("Big Three Dragons"), a bright Lyman-break galaxy system ($M_\text{UV}=-22.5$ mag) at $z=7.15$. The high angular resolution of NIRCam reveals the complex morphology of two galaxy components: galaxy E has a compact core (E-core), surrounded by diffuse, extended, rest-frame optical emission, which is likely to be tidal tails; and galaxy W has a clumpy and elongated morphology with a blue UV slope ($β_\text{UV}=-2.2\pm0.1$). The flux excess, F356W$-$F444W, peaks at the E-core ($1.05^{+0.08}_{-0.09}$ mag), tracing the presence of strong [OIII] 4960,5008 Å emission. ALMA archival data show that the bluer galaxy W is brighter in dust continua than the redder galaxy E, while the tails are bright in [OIII] 88 $\mathrm{μm}$. The UV/optical and sub-mm SED fitting confirms that B14-65666 is a major merger in a starburst phase as derived from the stellar mass ratio (3:1 to 2:1) and the star-formation rate, $\simeq1$ dex higher than the star-formation main sequence at the same redshift. The galaxy E is a dusty ($A_\text{V}=1.2\pm0.1$ mag) starburst with a possible high dust temperature ($\ge63$-$68$ K). The galaxy W would have a low dust temperature ($\le27$-$33$ K) or patchy stellar-and-dust geometry, as suggested from the infrared excess (IRX) and $β_\text{UV}$ diagram. The high optical-to-FIR [OIII] line ratio of the E-core shows its lower gas-phase metallicity ($\simeq0.2$-$0.4$ Z$_{\odot}$) than the galaxy W. These results agree with a scenario where major mergers disturb morphology and induce nuclear dusty starbursts triggered by less-enriched inflows. B14-65666 shows a picture of complex stellar buildup processes during major mergers in the epoch of reionization. |
| title | RIOJA. Complex Dusty Starbursts in a Major Merger B14-65666 at z=7.15 |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2403.17133 |