Abstract:The search of extragalactic regions with conspicuous presence of Wolf-Rayet (WR) stars outside the Local Group is challenging task owing to the difficulty in detecting their faint spectral features. In this exploratory work, we develop a methodology to perform an automated search of WR signatures through a pixel-by-pixel analysis of integral field spectroscopy (IFS) data belonging to the Calar Alto Legacy Integral Field Area survey, CALIFA. This procedure has been applied to a sample of nearby galaxies spannin… Show more
“…He iiλ4686/Hβ vs. [N ii]λ6584/Hα diagram of the local analogues of high-redshift galaxies (blue data points) and the SDSS reference galaxies (red data points). The black lines are the best-fit Gaussian Models of the emission lines spectra are narrow with σ = 100 − 200 km s −1 with no obvious broad component, associated with strong Wolf-Rayet stars (e.g.,Miralles-Caballero et al 2016). …”
We study the physical mechanisms that cause the offset between low-redshift and highredshift galaxies on the [O iii]λ5007/Hβ versus [N ii]λ6584/Hα "Baldwin, Phillips & Terlevich" (BPT) diagram using a sample of local analogues of high-redshift galaxies. These high-redshift analogue galaxies are selected from the Sloan Digital Sky Survey. Located in the same region on the BPT diagram as the ultra-violet selected galaxies at z ∼ 2, these high-redshift analogue galaxies provide an ideal local benchmark to study the offset between the local and high-redshift galaxies on the BPT diagram. We compare the nitrogen-to-oxygen ratio (N/O), the shape of the ionising radiation field, and ionisation parameters between the high-redshift analogues and a sample of local reference galaxies. The higher ionisation parameter in the high-redshift analogues is the dominant physical mechanism driving the BPT offset from low-to high-redshift, particularly at high [N ii]λ6584/Hα. Furthermore, the N/O ratio enhancement also plays a minor role to cause the BPT offset. However, the shape of the ionising radiation field is unlikely to cause the BPT offset because the high-redshift analogues have a similar hard ionising radiation field as local reference galaxies. This hard radiation field cannot be produced by the current standard stellar synthesis models. The stellar rotation and binarity may help solve the discrepancy.
“…He iiλ4686/Hβ vs. [N ii]λ6584/Hα diagram of the local analogues of high-redshift galaxies (blue data points) and the SDSS reference galaxies (red data points). The black lines are the best-fit Gaussian Models of the emission lines spectra are narrow with σ = 100 − 200 km s −1 with no obvious broad component, associated with strong Wolf-Rayet stars (e.g.,Miralles-Caballero et al 2016). …”
We study the physical mechanisms that cause the offset between low-redshift and highredshift galaxies on the [O iii]λ5007/Hβ versus [N ii]λ6584/Hα "Baldwin, Phillips & Terlevich" (BPT) diagram using a sample of local analogues of high-redshift galaxies. These high-redshift analogue galaxies are selected from the Sloan Digital Sky Survey. Located in the same region on the BPT diagram as the ultra-violet selected galaxies at z ∼ 2, these high-redshift analogue galaxies provide an ideal local benchmark to study the offset between the local and high-redshift galaxies on the BPT diagram. We compare the nitrogen-to-oxygen ratio (N/O), the shape of the ionising radiation field, and ionisation parameters between the high-redshift analogues and a sample of local reference galaxies. The higher ionisation parameter in the high-redshift analogues is the dominant physical mechanism driving the BPT offset from low-to high-redshift, particularly at high [N ii]λ6584/Hα. Furthermore, the N/O ratio enhancement also plays a minor role to cause the BPT offset. However, the shape of the ionising radiation field is unlikely to cause the BPT offset because the high-redshift analogues have a similar hard ionising radiation field as local reference galaxies. This hard radiation field cannot be produced by the current standard stellar synthesis models. The stellar rotation and binarity may help solve the discrepancy.
“…Hence, a prominent broad He ii component is expected for a Wolf-Rayet galaxy in which such stars are a significant population (e.g. Brinchmann et al 2008;Miralles-Caballero et al 2016;Liang et al 2020). The He ii line detected with MUSE for Jil2 is narrow instead, with a FWHM of only ∼ 300km s −1 , as characterised in Paper I, and therefore is incompatible with a traditional Wolf-Rayet galaxy interpretation.…”
Section: The Origin Of He II λ1640 Emission In Jil2mentioning
Context. Contrary to expectations from scenarios of black hole growth driven by galaxy interactions and mergers, dual active galactic nuclei (AGN) with kiloparsec separations are rarely observed and are very difficult to identify, in particular at high redshifts (i.e. z > 2). Aims. Focussing on the recently discovered dual AGN system LBQS 0302−0019 at z = 3.29, we seek to identify further group members in its environment and to understand their formation history through deep high-angular-resolution imaging. Methods. We present deep Hubble Space Telescope (HST) Wide-field Camera 3 near-infrared imaging of LBQS 0302−0019. In combination with ground-based VLT/HAWK-I imaging, we infer accurate sizes, colours, ages, and stellar masses of companion galaxies.Results. We clearly detect four companion objects close to LBQS 0302−0019 that also have faint signatures in the ground-based images. We constrain light-weighted ages and masses for the two most prominent companions, Jil1 and Jil2, to t = 252 +222 −109 Myr with log(M /[M ]) = 11.2 +0.3 −0.1 and t = 19 +74 −14 Myr with log(M /[M ]) = 9.4 +0.9 −0.4 , respectively. The HST data also show that the obscured AGN, previously identified by strong nebular He ii emission, is associated with the young massive companion Jil2. Because very massive stars of the starburst cannot be solely responsible for the He ii emission, we strengthen our initial conclusion that Jil2 has been hosting an AGN. Conclusions. If the young starburst of Jil2 had been accompanied by sustained black hole growth, Jil2 may have contributed He iiionising flux to create the large He ii Lyα proximity zone around LBQS 0302−0019. Hence, the duration of the current luminous AGN episode of LBQS 0302−0019 may have been overestimated.
“…Both NGC 3773 and NGC 7077 have central blue features that are classified as H II regions, which are probably caused by Wolf-Rayet stars (Miralles-Caballero et al 2016).…”
We present and analyze spatially-resolved maps for the observed V -and g-band to 3.6 µm flux ratios and the inferred dust extinction values, A V , for a sample of 257 nearby NGC and IC galaxies. Flux ratio maps are constructed using PSF-matched mosaics of SDSS gand r-band images and Spitzer/IRAC 3.6 µm mosaics, with all pixels contaminated by foreground stars or background objects masked out. By applying the β V method (Tamura et al. 2009(Tamura et al. , 2010, which was recently calibrated as a function of redshift and morphological type by Kim, Jansen, & Windhorst (2017), dust extinction maps were created for each galaxy. The typical 1-σ scatter in β V around the average, both within a galaxy and in each morphological type bin, is ∼20%. Combined, these result in a ∼0.4 mag scatter in A V . β V becomes insensitive to small-scale variations in stellar populations once resolution elements subtend an angle larger than that of a typical giant molecular cloud (∼200 pc). We find noticeably redder V −3.6 µm colors in the center of star-forming galaxies and galaxies with a weak AGN. The derived intrinsic V −3.6 µm colors for each Hubble type are generally consistent with the model predictions of Kim et al. (2017). Finally, we discuss the applicability of the β V dust-correction method to more distant galaxies, for which well-matched HST rest-frame visible and JWST rest-frame ∼3.5µm images will become available in the near-future.
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