We present average stellar population properties and dark matter halo masses of z \sim 2 { Ly } \alpha emitters ( LAEs ) \color blackfrom SED fitting and clustering analysis , respectively , \color blackusing \simeq 1250 objects ( NB 387 \leq 25.5 ) in four separate fields of \simeq 1 deg ^ { 2 } in total .
With an average stellar mass of \color black 10.2 \pm 1.8 \times 10 ^ { 8 } { \mathrm { M } _ { \odot } } and star formation rate of \color black 3.4 \pm 0.4 { \mathrm { M } _ { \odot } } { yr ^ { -1 } } , the LAEs \color blacklie on an extrapolation of the star-formation main sequence ( MS ) to low stellar mass .
Their effective dark matter halo mass is estimated to be 4.0 _ { -2.9 } ^ { +5.1 } \times 10 ^ { 10 } { \mathrm { M } _ { \odot } } with \color black an effective bias of 1.22 ^ { +0.16 } _ { -0.18 } \color blackwhich is lower than that of z \sim 2 LAEs \color black ( 1.8 \pm 0.3 ) , obtained by a previous study based on a three times smaller \color blacksurvey area , with a probability of 96 \% . \color blackHowever , the difference in the bias values can be explained if cosmic variance is taken into account .
If such a low halo mass implies a low HI gas mass , this result appears to be consistent with the observations of a high { Ly } \alpha escape fraction . \color blackWith the low halo masses and ongoing star formation , our LAEs have a relatively high stellar-to-halo mass ratio ( SHMR ) and a high efficiency of converting baryons into stars .
The extended Press-Schechter formalism predicts that at z = 0 our LAEs are typically embedded in halos with masses similar to that of the Large Magellanic Cloud ( LMC ) ; \color blackthey will also have similar SHMRs to the LMC , if their SFRs are largely suppressed after z \sim 2 as some previous studies have reported for the LMC itself .