Explore the vast range of titles available.

When the Universe was just 3 billion years old, half of the most massive galaxies had already ceased star formation, and such a galaxy has now been observed using gravitational lensing, unexpectedly turning out to be a compact, fast-spinning disk galaxy rather than a proto-bulge galaxy. Dead disk galaxy formed by incoming gas When the Universe was only three billion years old, half of the most massive galaxies were already 'dead', meaning that few new stars would form in them. It is believed that these galaxies grew into the massive local elliptical galaxies seen today. Sune Toft et al . report an analysis of a galaxy that has been strongly gravitationally lensed. This means that they can observe spatial scales that are far smaller than those accessible by any other means. They find that, surprisingly, the galaxy is a fast-spinning disk and that its stars formed in situ rather than in a nuclear starburst. They conclude that the gas out of which the stars formed was accreted from outside the galaxy in cold streams of gas. At redshift z  = 2, when the Universe was just three billion years old, half of the most massive galaxies were extremely compact and had already exhausted their fuel for star formation 1 , 2 , 3 , 4 . It is believed that they were formed in intense nuclear starbursts and that they ultimately grew into the most massive local elliptical galaxies seen today, through mergers with minor companions 5 , 6 , but validating this picture requires higher-resolution observations of their centres than is currently possible. Magnification from gravitational lensing offers an opportunity to resolve the inner regions of galaxies 7 . Here we report an analysis of the stellar populations and kinematics of a lensed z  = 2.1478 compact galaxy, which—surprisingly—turns out to be a fast-spinning, rotationally supported disk galaxy. Its stars must have formed in a disk, rather than in a merger-driven nuclear starburst 8 . The galaxy was probably fed by streams of cold gas, which were able to penetrate the hot halo gas until they were cut off by shock heating from the dark matter halo 9 . This result confirms previous indirect indications 10 , 11 , 12 , 13 that the first galaxies to cease star formation must have gone through major changes not just in their structure, but also in their kinematics, to evolve into present-day elliptical galaxies.

At z=2, when the Universe was just 3 Gyr old, half of the most massive galaxies were extremely compact and had already exhausted their fuel for star formation1–4. It is believed that they were formed in intense nuclear starbursts and that they ultimately grew into the most massive local elliptical galaxies seen today, through mergers with minor companions5,6, but validating this scenario requires higher resolution observations of their centers than currently possible, even from space. Magnification due to gravitational lensing offers a unique opportunity to resolve their inner regions, as demonstrated in a recent study of a z=2.6 compact spheroidal galaxy which revealed a bulge, rotating at velocities comparable to the fastest rotating local ellipticals7. Following the same approach, here we map the stellar populations and kinematics of a lensed z=2.1478 compact galaxy, which surprisingly turn out to be a fast spinning, rotationally supported disk galaxy. Rather than in a merger-driven nuclear starburst8, its stars must thus have formed in a disk, likely fed by streams of cold gas, which were able to penetrate the hot halo gas until they were cut off by shock heating from the dark matter halo9. This result unambiguously confirm indications from a growing body of indirect evidence10–13 that the first galaxies to cease star formation must go through major changes not just in their structure, but also in their kinematics to evolve into present day ellipticals.

When the Universe was just 3 billion years old, half of the most massive galaxies had already ceased star formation, and such a galaxy has now been observed using gravitational lensing, unexpectedly turning out to be a compact, fast-spinning disk galaxy rather than a proto-bulge galaxy.

This work presents an in-depth analysis of four gravitationally lensed red galaxies at z = 1.6-3.2. The sources are magnified by factors of 2.7-30 by foreground clusters, enabling spectral and morphological measurements that are otherwise challenging. Our sample extends below the characteristic mass of the stellar mass function and is thus more representative of the quiescent galaxy population at z > 1 than previous spectroscopic studies. We analyze deep VLT/X-SHOOTER spectra and multi-band Hubble Space Telescope photometry that cover the rest-frame UV-to-optical regime. The entire sample resembles stellar disks as inferred from lensing-reconstructed images. Through stellar population synthesis analysis we infer that the targets are young (median age = 0.1-1.2 Gyr) and formed 80% of their stellar masses within 0.07-0.47 Gyr. Mg II \\(\\lambda\\lambda 2796,2803\\) absorption is detected across the sample. Blue-shifted absorption and/or redshifted emission of Mg II is found in the two youngest sources, indicative of a galactic-scale outflow of warm (\\(T\\sim10^{4}\\) K) gas. The [O III] \\(\\lambda5007\\) luminosity is higher for the two young sources (median age less than 0.4 Gyr) than the two older ones, perhaps suggesting a decline in nuclear activity as quenching proceeds. Despite high-velocity (\\(v\\approx1500\\) km s\\(^{-1}\\)) galactic-scale outflows seen in the most recently quenched galaxies, warm gas is still present to some extent long after quenching. Altogether our results indicate that star formation quenching at high redshift must have been a rapid process (< 1 Gyr) that does not synchronize with bulge formation or complete gas removal. Substantial bulge growth is required if they are to evolve into the metal-rich cores of present-day slow-rotators.

We examine the Fundamental Plane (FP) and mass-to-light ratio (\\(M/L\\)) scaling relations using the largest sample of massive quiescent galaxies at \\(1.511.26\\), subset of 8 quiescent galaxies at \\(z>2\\), from Stockmann et al. (2020), we show that they cannot passively evolve to the local Coma cluster relation alone and must undergo significant structural evolution to mimic the sizes of local massive galaxies. The evolution of the FP and \\(M/L\\) scaling relations, from \\(z=2\\) to present-day, for this subset are consistent with passive aging of the stellar population and minor merger structural evolution into the most massive galaxies in the Coma cluster and other massive elliptical galaxies from the MASSIVE Survey. Modeling the luminosity evolution from minor merger added stellar populations favors a history of merging with \"dry\" quiescent galaxies.

We present the first stellar velocity dispersion measurement of a massive quenching galaxy at z=4.01. The galaxy is first identified as a massive z>~4 galaxy with suppressed star formation from photometric redshifts based on deep multi-band data in the UKIDSS Ultra Deep Survey field. A follow-up spectroscopic observation with MOSFIRE on Keck revealed strong multiple absorption features, which are identified as Balmer absorption lines, giving a secure redshift of z=4.01. Thanks to the high S/N of the spectrum, we are able to estimate the stellar velocity dispersion, sigma=268+/-59 km/s. This velocity dispersion is consistent with that of massive galaxies today, implying no significant evolution in stellar velocity dispersion over the last 12 Gyr. Based on an upper limit on its physical size from deep optical images (r_eff<1.3 kpc), we find that its dynamical mass is consistent with the stellar mass inferred from photometry. Furthermore, the galaxy is located on the mass fundamental plane extrapolated from lower redshift galaxies. Combining all these results, we find that the velocity dispersion does not significantly evolve with redshift, although the size and mass of massive quenched galaxies do. This suggests that the mass in the core of massive galaxies does not evolve significantly, while most of the mass growth occurs in the outskirts of the galaxies, which also increases the size. This picture is consistent with a two-phase formation scenario in which mass and size growth is due to accretion in the outskirts of galaxies via mergers.

Most molecular gas studies of \\(z > 2.5\\) galaxies are of intrinsically bright objects, despite the galaxy population being primarily \"normal\" galaxies with less extreme star formation rates. Observations of normal galaxies at high redshift provide a more representative view of galaxy evolution and star formation, but such observations are challenging to obtain. In this work, we present ALMA \\(\\rm ^{12}CO(J = 3 \\rightarrow 2)\\) observations of a sub-millimeter selected galaxy group at \\(z = 2.9\\), resulting in spectroscopic confirmation of seven images from four member galaxies. These galaxies are strongly lensed by the MS 0451.6-0305 foreground cluster at \\(z = 0.55\\), allowing us to probe the molecular gas content on levels of \\(\\rm 10^9-10^{10} \\; M_\\odot\\). Four detected galaxies have molecular gas masses of \\(\\rm (0.2-13.1) \\times 10^{10} \\; M_\\odot\\), and the non-detected galaxies have inferred molecular gas masses of \\(\\rm < 8.0 \\times 10^{10} \\; M_\\odot\\). We compare these new data to a compilation of 546 galaxies up to \\(z = 5.3\\), and find that depletion times decrease with increasing redshift. We then compare the depletion times of galaxies in overdense environments to the field scaling relation from the literature, and find that the depletion time evolution is steeper for galaxies in overdense environments than for those in the field. More molecular gas measurements of normal galaxies in overdense environments at higher redshifts (\\(z > 2.5\\)) are needed to verify the environmental dependence of star formation and gas depletion.

We report two secure (\\(z=3.775, 4.012\\)) and one tentative (\\(z\\approx3.767\\)) spectroscopic confirmations of massive and quiescent galaxies through \\(K\\)-band observations with Keck/MOSFIRE and VLT/X-Shooter. The stellar continuum emission, the absence of strong nebular emission lines and the lack of significant far-infrared detections confirm the passive nature of these objects, disfavoring the alternative solution of low-redshift dusty star-forming interlopers. We derive stellar masses of \\(\\mathrm{log}(M_{\\star}/M_\\odot)\\sim11\\) and ongoing star formation rates placing these galaxies \\(\\gtrsim 1-2\\) dex below the main sequence at their redshifts. The adopted parametrization of the star formation history suggests that these sources experienced a strong (\\(\\langle \\rm SFR \\rangle \\sim 1200-3500\\,M_\\odot\\,\\mathrm{yr}^{-1}\\)) and short (\\(\\sim 50\\) Myr) burst of star formation, peaking \\(\\sim 150-500\\) Myr before the time of observation, all properties reminiscent of the characteristics of sub-millimeter galaxies (SMGs) at \\(z>4\\). We investigate this connection by comparing the comoving number densities and the properties of these two populations. We find a fair agreement only with the deepest sub-mm surveys detecting not only the most extreme starbursts, but also more normal galaxies. We support these findings by further exploring the Illustris-TNG cosmological simulation, retrieving populations of both fully quenched massive galaxies at \\(z\\sim3-4\\) and SMGs at \\(z\\sim4-5\\), with number densities and properties in agreement with the observations at \\(z\\sim3\\), but in increasing tension at higher redshift. Nevertheless, as suggested by the observations, not all the progenitors of quiescent galaxies at these redshifts shine as bright SMGs in their past and, similarly, not all bright SMGs quench by \\(z\\sim3\\), both fractions depending on the threshold assumed to define the SMGs themselves.

We present the rest-frame optical sizes of massive quiescent galaxies (QGs) at \\(z\\sim4\\) measured at \\(K'\\)-band with the Infrared Camera and Spectrograph (IRCS) and AO188 on the Subaru telescope. Based on a deep multi-wavelength catalog in the Subaru XMM-Newton Deep Survey Field (SXDS), covering a wide wavelength range from the \\(u\\)-band to the IRAC \\(8.0\\mu m\\) over 0.7 deg\\(^2\\), we evaluate photometric redshift to identify massive (\\(M_{\\star}\\sim10^{11}\\ M_\\odot\\)) galaxies with suppressed star formation. These galaxies show a prominent 4000\\(\\rm \\AA\\) break feature at \\(z\\sim4\\), suggestive of an evolved stellar population. We then conduct follow-up \\(K'\\)-band imaging with adaptive optics for the five brightest galaxies (\\(K_{AB,total}=22.5\\sim23.4\\)). Compared to lower redshift ones, QGs at \\(z\\sim4\\) have smaller physical sizes of effective radii \\(r_{eff}=0.2\\) to \\(1.8\\) kpc. The mean size measured by stacking the four brightest objects is \\(r_{eff}=0.7\\rm\\ kpc\\). This is the first measurement of the rest-frame optical sizes of QGs at \\(z\\sim4\\). We evaluate the robustness of our size measurements using simulations and find that our size estimates are reasonably accurate with an expected systematic bias of \\(\\sim0.2\\) kpc. If we account for the stellar mass evolution, massive QGs at \\(z\\sim4\\) are likely to evolve into the most massive galaxies today. We find their size evolution with cosmic time in a form of \\(\\log(r_e/{\\rm kpc})= -0.44+1.77 \\log(t/\\rm Gyr)\\). Their size growth is proportional to the square of stellar mass, indicating the size-stellar mass growth driven by minor dry mergers.

At redshift z = 2, when the Universe was just three billion years old, half of the most massive galaxies were extremely compact and had already exhausted their fuel for star formation(1-4). It is believed that they were formed in intense nuclear starbursts and that they ultimately grew into the most massive local elliptical galaxies seen today, through mergers with minor companions(5,6), but validating this picture requires higher-resolution observations of their centres than is currently possible. Magnification from gravitational lensing offers an opportunity to resolve the inner regions of galaxies(7). Here we report an analysis of the stellar populations and kinematics of a lensed z = 2.1478 compact galaxy, which surprisingly turns out to be a fast-spinning, rotationally supported disk galaxy. Its stars must have formed in a disk, rather than in a merger-driven nuclear starburst(8). The galaxy was probably fed by streams of cold gas, which were able to penetrate the hot halo gas until they were cut off by shock heating from the dark matter halo(9). This result confirms previous indirect indications(10-13) that the first galaxies to cease star formation must have gone through major changes not just in their structure, but also in their kinematics, to evolve into present-day elliptical galaxies.