اشترك بالحزمة الذهبية واحصل على وصول غير محدود شمرا أكاديميا
تسجيل مستخدم جديدA strong-lensing elliptical galaxy in the MaNGA survey
64
0
0.0
(
0
)
تأليف
Russell J. Smith
اسأل ChatGPT حول البحث
ﻻ يوجد ملخص باللغة العربية
I report discovery of a new galaxy-scale gravitational lens system, identified using public data from the MaNGA survey, as part of a systematic search for lensed background line-emitters. The lens is SDSS J170124.01+372258.0, a giant elliptical galaxy with velocity dispersion $sigma=256$ km/s, at a redshift of $z_l=0.122$. After modelling and subtracting the target galaxy light, the integral-field data-cube reveals [OII], [OIII] and H$beta$ emission lines corresponding to a source at $z_s=0.791$, forming an identifiable ring around the galaxy center. The Einstein radius is $R_{Ein} approx 2.3$ arcsec, projecting to ~5 kpc at the distance of the lens. The total projected lensing mass is $(3.6pm0.6) times 10^{11} M_odot$, and the total J-band mass-to-light ratio is $3.0pm0.7$ solar units. Plausible estimates of the likely dark matter content could reconcile this with a Milky-Way-like initial mass function (for which M/L~1.5 is expected), but heavier IMFs are by no means excluded with the present data. An alternative interpretation of the system, with a more complex source plane, is also discussed. The discovery of this system bodes well for future lens searches based on MaNGA and other integral-field spectroscopic surveys.
قيم البحث
اقرأ أيضاً
We report the discovery of a new low-redshift galaxy-scale gravitational lens, identified from a systematic search of publicly available MUSE observations. The lens galaxy, 2MASXJ04035024-0239275, is a giant elliptical at $z$ = 0.06604 with a velocit
y dispersion of $sigma$ = 314 km s$^{-1}$. The lensed source has a redshift of 0.19165 and forms a pair of bright images either side of the lens centre. The Einstein radius is 1.5 arcsec, projecting to 1.8 kpc, which is just one quarter of the galaxy effective radius. After correcting for an estimated 19 per cent dark matter contribution, we find that the stellar mass-to-light ratio from lensing is consistent with that expected for a Milky Way initial mass function (IMF). Combining the new system with three previously-studied low-redshift lenses of similar $sigma$, the derived mean mass excess factor (relative to a Kroupa IMF) is $langlealpharangle$ = 1.09$pm$0.08. With all four systems, the intrinsic scatter in $alpha$ for massive elliptical galaxies can be limited to $<0.32$, at 90 per cent confidence.
We present new observations of two z=0.12 strong-lensing elliptical galaxies, originally discovered from the SDSS-IV MaNGA survey, using the new FOCAS IFU spectrograph on the Subaru Telescope. For J1436+4943, our observations confirm the identificati
on of this system as a multiple-image lens, in a cusp configuration, with Einstein radius $theta_{Ein}$=2.0 arcsec. For J1701+3722, the improved data confirm earlier hints of a complex source plane, with different configurations evident in different emission lines. The new observations reveal a previously unseen inner counter-image to the [OIII] arc found from MaNGA, leading to a smaller revised Einstein radius of $theta_{Ein}$=1.6 arcsec. The inferred projected masses within the Einstein apertures (3.7-4.7kpc) are consistent with being dominated by stars with an initial mass function (IMF) similar to that of the Milky Way, and a dark matter contribution of ~35 per cent as supported from cosmological simulations. These results are consistent with `pure lensing analyses of lower-redshift lenses, but contrast with claims for heavier IMFs from combined lensing-and-dynamical studies of more distant early-type galaxies.
We investigate how strong gravitational lensing can test contemporary models of massive elliptical (ME) galaxy formation, by combining a traditional decomposition of their visible stellar distribution with a lensing analysis of their mass distributio
n. As a proof of concept, we study a sample of three ME lenses, observing that all are composed of two distinct baryonic structures, a `red central bulge surrounded by an extended envelope of stellar material. Whilst these two components look photometrically similar, their distinct lensing effects permit a clean decomposition of their mass structure. This allows us to infer two key pieces of information about each lens galaxy: (i) the stellar mass distribution (without invoking stellar populations models) and (ii) the inner dark matter halo mass. We argue that these two measurements are crucial to testing models of ME formation, as the stellar mass profile provides a diagnostic of baryonic accretion and feedback whilst the dark matter mass places each galaxy in the context of LCDM large scale structure formation. We also detect large rotational offsets between the two stellar components and a lopsidedness in their outer mass distributions, which hold further information on the evolution of each ME. Finally, we discuss how this approach can be extended to galaxies of all Hubble types and what implication our results have for studies of strong gravitational lensing.
We present the initial results of a census of 684 barred galaxies in the MaNGA galaxy survey. This large sample contains galaxies with a wide range of physical properties, and we attempt to link bar properties to key observables for the whole galaxy.
We find the length of the bar, when normalised for galaxy size, is correlated with the distance of the galaxy from the star formation main sequence, with more passive galaxies hosting larger-scale bars. Ionised gas is observed along the bars of low-mass galaxies only, and these galaxies are generally star-forming and host short bars. Higher-mass galaxies do not contain H{alpha} emission along their bars, however, but are more likely to host rings or H{alpha} at the centre and ends of the bar. Our results suggest that different physical processes are at play in the formation and evolution of bars in low- and high-mass galaxies.
Pressure supported systems modeled under MONDian extended gravity are expected to show an outer flattening in their velocity dispersion profiles. A characteristic scaling between the amplitude of the asymptotic velocity dispersion and the radius at w
hich the flattening occurs is also expected. By comprehensively analyzing the dynamical behavior of $sim$300 extremely low rotating elliptical galaxies from the MaNGA survey, we show this type of pressure supported systems to be consistent with MONDian expectations, for a range of central velocity dispersion values of $60 km/s < sigma_{central}< 280 km/s $ and asymptotic velocity dispersion values of $28km/s < sigma_{infty}<250 km/s$. We find that a universal velocity dispersion profile accurately describes the studied systems; the predicted kinematics of extended gravity are verified for all well observed galaxies.
سجل دخول لتتمكن من نشر تعليقات
التعليقات
جاري جلب التعليقات
سجل دخول لتتمكن من متابعة معايير البحث التي قمت باختيارها
