Consequences of bursty star formation on galaxy observables at high redshifts
Consequences of bursty star formation on galaxy observables at high redshifts
复制标题
爆发式恒星形成对高红移星系可观测值的影响
DOI：
10.1093/mnras/stv1001
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发表时间：
2014
影响因子：
4.8
通讯作者：
A. Alavi
中科院分区：
文献类型：
--
作者：
A. Domínguez;B. Siana;A. Brooks;C. Christensen;G. Bruzual;D. Stark;A. Alavi
矮星系的恒星形成历史(SFH)被认为是爆发的，具有大数量级的恒星形成速率在类似于O星寿命的时间尺度上的变化。因此，对许多星系可见天体的标准解释(假设SFH缓慢变化)往往是不正确的。在这里，我们使用水动力学模拟中的SFH来研究突发性SFH对样本选择和可观测数据解释的影响，并做出预测，以在未来的调查中证实这种SFH。首先，由于矮星系的恒星形成率变化很快，在电离连续体和非电离紫外光连续体中，质光比也在迅速变化，程度较小。因此，流量受限的调查高度偏向于选择爆发阶段的星系，需要非常深入的观测来探测给定恒星质量的所有矮小星系。其次，我们证明了LOG 10[νL�(1500u/Lh�]>；2.5暗示恒星形成最近的猝灭，可以作为恒星反馈调节恒星形成的证据。第三，我们发现电离连续谱比假设SFH恒定时要高得多，这会影响对星云发射线等效宽度和直接电离连续谱探测的解释。最后，我们表明，仅基于连续测量的恒星形成速率估计(而不是基于星云示踪物，如氢巴尔默线)将不会跟踪恒星形成的快速变化，并将给人一种低分散的恒星形成主序列的错误印象。
The star formation histories (SFHs) of dwarf galaxies are thought to be bursty, with large – order of magnitude – changes in the star formation rate on timescales similar to O-star lifetimes. As a result, the standard interpretations of many galaxy observables (which assume a slowly varying SFH) are often incorrect. Here, we use the SFHs from hydro-dynamical simulations to investigate the effects of bursty SFHs on sample selection and interpretation of observables and make predictions to confirm such SFHs in future surveys. First, because dwarf galaxies’ star formation rates change rapidly, the mass-to-light ratio is also changing rapidly in both the ionizing continuum and, to a lesser extent, the non-ionizing UV continuum. Therefore, flux limited surveys are highly biased toward selecting galaxies in the burst phase and very deep observations are required to detect all dwarf galaxies at a given stellar mass. Second, we show that a log 10 [νL�(1500u/LH�] > 2.5 implies a very recent quenching of star formation and can be used as evidence of stellar feedback regulating star formation. Third, we show that the ionizing continuum can be significantly higher than when assuming a constant SFH, which can affect the interpretation of nebular emission line equivalent widths and direct ionizing continuum detections. Finally, we show that a star formation rate estimate based on continuum measurements only (and not on nebular tracers such as the hydrogen Balmer lines) will not trace the rapid changes in star formation and will give the false impression of a star-forming main sequence with low dispersion.
WFC3 红外光谱平行 (WISP) 调查
DOI：
10.1088/0004-637x/723/1/104
发表时间：
2010
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Atek H
通讯作者：
Atek H
DOI：
10.1088/0004-6256/140/5/1194
发表时间：
2010-07
期刊：
The Astronomical Journal
影响因子：
--
作者：
F. Bigiel;A. Leroy;F. Walter;L. Blitz;E. Brinks;W. D. Blok;B. M. U. Berkeley;Mpia Heidelberg;Nrao;U. Hertfordshire;U. C. Town;C. Observatories
通讯作者：
F. Bigiel;A. Leroy;F. Walter;L. Blitz;E. Brinks;W. D. Blok;B. M. U. Berkeley;Mpia Heidelberg;Nrao;U. Hertfordshire;U. C. Town;C. Observatories
宇宙时间极端星暴的哈勃太空望远镜格里斯光谱：矮星系在宇宙恒星形成历史中的作用
DOI：
10.1088/0004-637x/789/2/96
发表时间：
2014
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Atek H
通讯作者：
Atek H