Galaxy (LAE) Catalogues

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(Last updated on 14/Oct/2021)

Contents

Overview

This project aims to model Lyman-alpha emitters (LAEs) to understand the formation and evolution of LAEs. Lyman-alpha emitters (LAEs) are known to be young and active star-forming galaxies. Since LAEs are less dusty, these are a good tracer of the underlying matter distribution. The predicted LAEs from the cosmological simulation will be compared with LAEs observed from One-hundred-square-degree DECam Imaging in Narrow band (ODIN) survey at z = 2.4, 3.1, and 4.5, which is conducting in the largest survey area of total ~91 deg2

Catalogues (based on HR5)

Catalogues include the rest-frame AB magnitudes at 1600Å (intrinsic and dust-attenuated, i.e. MUV, intrinsic and MUV, obs), the rest-frame equivalent widths (REWs), Ly-𝛼 luminosities (intrinsic and observed), as well as all the galaxy properties that HR5 provides.


*Note that the Catalogues will be available when you have permission from LASOR CoCo. To obtain permission, you are firstly required to submit a research proposal to LASOR CoCo.



The rest-frame Ly-𝛼 equivalent width distribution

Figure 5: the rest-frame Ly-𝛼 equivalent width distribution at z=2.4, 3.1 and 4.5, predicted from HR5. The histogram is calculated with bin size of 20Å. At each panel, red dotted lines represent the minimum REWs, which are 130Å (Konno et al. 2016) at z=2.4 and 64Å (Ouchi et al. 2008) at z=3.1, respectively.

LAE_EW_dist.png

Ly-𝛼 luminosity functions

Figure 4: Ly-𝛼 luminosity functions at z=2.4, 3.1, and 4.5. Grey and black lines represent the intrinsic and observed (i.e. applied the IGM absorption) Ly-𝛼 LFs, respectively. Colored lines represent LFs with assumed minimum equivalent widths (denoted as legends). At each panel, grey dotted lines indicate the detection limit of Ly-𝛼 luminosities when assuming the ODIN survey [log10(LLy-𝛼)min = 42.42, 42.17, and 42.21 at z=2.4, 3.1, and 4.5, respectively]. At z=2.4, the right side of the orange dotted line indicates the region that AGN contributions dominate (e.g., Matthee et al. 2017).

L_Lya_LFs.png

The rest-frame UV luminosity functions

Figure 3: The rest-frame UV luminosity functions (LFs) at z=2, 3, 4, and 5. The thin solid (grey) lines represent the intrinsic UV LFs. Thick solid, dashed, and dotted lines represent dust-corrected UV LFs of all galaxies, galaxies with M > 108M, and with M > 109M, respectively. Symbols with error bars represent observed LFs from various groups (see the legend). The observed LFs at each redshit are used to find the best-fit parameters for the dust-correction model.

LF_HR5_z2-5_Best-fit.png


Figure 2: The same as Figure 1, but at higher redshifts, i.e. z=6, 7, 8, 9, and 10.

UVLFs_HR5_z6-10.png


Figure 1: Best-fit parameters to fit predicted LFs to observed LFs at various redshifts. Cross (red) symbols represent best-fit parameters found in HR5. Plus (black) symbols found in Illustris TNG simulations are plotted together for comparison. Circles, squares, and stars with error bars are estimated parameters from Bouwens et al. (2012), Bouwens et al. (2014), and Finkelstein et al. (2012), respectively.

BestFitParams.png

Details are in the file below.

Presentation 16May2022

Presentation 17Nov2021

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