A refined mass distribution of the cluster MACS J0416.1−2403 from a new large set of spectroscopic multiply lensed sources

Caminha, G. B.; Grillo, C.; Rosati, P.; Balestra, I.; Mercurio, A.; Vanzella, E.; Biviano, A.; Caputi, K.; Delgado-Correal, Camilo; Karman, W.; Lombardi, Marco; Meneghetti, M.; Sartoris, B.; Tozzi, P.

doi:10.1051/0004-6361/201629297

Cited by 134 publications

(169 citation statements)

References 75 publications

(114 reference statements)

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“…Stellar mass density profiles were estimated from the stellar mass of each BCG assuming a Hernquist (1990) profile and the Shen et al (2003) mass-size relationship (Ruszkowski & Springel 2009;Laporte et al 2013). The inclusion of stellar mass in our estimates of M enc (r) does not significantly affect the freefall time profiles at radii 25 kpc (or similarly 0.025R 500 ), which is not surprising given that BCG stellar mass dominates the cluster density profile only within the central ∼ 10 kpc of a cluster (Newman et al 2013;Monna et al 2017;Caminha et al 2017). Still, we include the BCG stellar mass in our estimation of the free-fall time profiles and find that the BCG stellar masses alter the free fall times by 4% at ∼ 10 kpc and 1% at ∼ 20 kpc.…”

Section: Cooling and Freefall Time Profilesmentioning

confidence: 58%

The Relationship Between Brightest Cluster Galaxy Star Formation and the Intracluster Medium in CLASH

Fogarty

Postman

Larson

et al. 2017

ApJ

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We study the nature of feedback mechanisms in the 11 CLASH brightest cluster galaxies (BCGs) that exhibit extended ultraviolet and nebular line emission features. We estimate star formation rates (SFRs), dust masses, and starburst durations using a Bayesian photometry-fitting technique that accounts for both stellar and dust emission from the UV through far IR. By comparing these quantities to intracluster medium (ICM) cooling times and free-fall times derived from X-ray observations and lensing estimates of the cluster mass distribution, we discover a tight relationship between the BCG SFR and the ICM cooling time to free-fall time ratio, t cool /t f f , with an upper limit on the intrinsic scatter of 0.15 dex. Furthermore, starburst durations may correlate with ICM cooling times at a radius of 0.025R 500 , and the two quantities converge upon reaching the Gyr regime. Our results provide a direct observational link between the thermodynamical state of the ICM and the intensity and duration of BCG star formation activity, and appear consistent with a scenario where active galactic nuclei (AGN) induce condensation of thermally unstable ICM overdensities that fuel longduration (> 1 Gyr) BCG starbursts. This scenario can explain (a) how gas with a low cooling time is depleted without causing a cooling flow and (b) the scaling relationship between SFR and t cool /t f f . We also find that the scaling relation between SFR and dust mass in BCGs with SFRs < 100 M yr −1 is similar to star-forming field galaxies; BCGs with large (> 100 M yr −1 ) SFRs have dust masses comparable to extreme starbursts.

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Section: Cooling and Freefall Time Profilesmentioning

confidence: 58%

The Relationship Between Brightest Cluster Galaxy Star Formation and the Intracluster Medium in CLASH

Fogarty

Postman

Larson

et al. 2017

ApJ

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“…Interestingly, 10 of the 27 multiply imaged sources are Lyman-α emitters with no detection in the CLASH imaging data (limiting AB mag in F814W = 27.7), illustrating the high sensitivity of MUSE to emission lines. We note that Lyman-α emitters with no imaging counterpart have been found with MUSE even in deeper HST imaging, such as in the Hubble Frontier Fields (see, e.g., Caminha et al 2017;Mahler et al 2017). Although they are very faint, the images of these sources are clearly detected in the MUSE data-cube and their spectroscopic redshifts are secure (see Fig.…”

Section: Multiple Image Identificationmentioning

confidence: 78%

“…The raw data were reduced using the standard calibrations provided by the MUSE pipeline (Weilbacher et al 2014), version 1.6.2, following the same procedures described in Caminha et al (2017). For each of the 25 observations we checked the calibrated data-cube and wavelength-collapsed images, but did not find large variations on the observational conditions and final calibration.…”

Section: Muse Observationsmentioning

confidence: 99%

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Mass distribution in the core of MACS J1206

Caminha

Grillo

Rosati

et al. 2017

A&A

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We present a new strong lensing analysis of the galaxy cluster MACS J1206.2−0847 (MACS 1206), at z = 0.44, using deep spectroscopy from CLASH-VLT and VLT/MUSE archival data in combination with imaging from the Cluster Lensing and Supernova survey with Hubble. MUSE observations enable the spectroscopic identification of 23 new multiply imaged sources, extending the previous compilations by a factor of approximately five. In total, we use the positional measurements of 82 spectroscopic multiple images belonging to 27 families at z = 1.0 − 6.1 to reconstruct the projected total mass distribution of MACS 1206. Remarkably, 11 multiple images are found within 50 kpc of the brightest cluster galaxy, making this an unprecedented set of constraints for the innermost projected mass distribution of a galaxy cluster. We thus find that, although dynamically relaxed, the smooth matter component (dark matter plus hot gas) of MACS 1206 shows a significant asymmetry, which closely follows the asymmetric distribution of the stellar component (galaxy members and intracluster light). We determine the value of the innermost logarithmic slope of the projected total mass density profile and find it to be close to the canonical Navarro-Frenk-White value. We demonstrate that this quantity is very robust against different parametrizations of the diffuse mass component; however, this is not the case when only one central image is used in the mass reconstruction. We also show that the mass density profile from our new strong lensing model is in very good agreement with dynamical and X-ray measurements at larger radii, where they overlap.

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“…In this work, we exploit MUSE archival data obtained from two different programs which covered the North-East (NE) and South-West (SW) regions of the cluster. A detailed description of the MUSE data reduction and analysis is given in Caminha et al (2017). Here, we use the sample of cluster members also considered in Bonamigo et al (2017, hereafter Bo17), including 193 galaxies, 144 with spectroscopic redshifts, and the others selected based on their N -dimensional distance, in color space, from the locus of the spectroscopically confirmed member galaxies (see Grillo et al 2015, for more details).…”

Section: Data Samplementioning

confidence: 99%

Mass Profile Decomposition of the Frontier Fields Cluster MACS J0416-2403: Insights on the Dark-matter Inner Profile

Annunziatella

Bonamigo

Grillo

et al. 2017

ApJ

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We present a high resolution dissection of the two-dimensional total mass distribution in the core of the Hubble Frontier Fields galaxy cluster MACS J0416.1−2403, at z = 0.396. We exploit HST/WFC3 near-IR (F160W) imaging, VLT/MUSE spectroscopy, and Chandra data to separate the stellar, hot gas, and dark-matter mass components in the inner 300 kpc of the cluster. We combine the recent results of our refined strong lensing analysis, which includes the contribution of the intracluster gas, with the modeling of the surface brightness and stellar mass distributions of 193 cluster members, of which 144 are spectroscopically confirmed. We find that moving from 10 to 300 kpc from the cluster center the stellar to total mass fraction decreases from 12% to 1% and the hot gas to total mass fraction increases from 3% to 9%, resulting in a baryon fraction of approximatively 10% at the outermost radius. We measure that the stellar component represents ∼ 30%, near the cluster center, and 15%, at larger clustercentric distances, of the total mass in the cluster substructures. We subtract the baryonic mass component from the total mass distribution and conclude that within 30 kpc (∼ 3 times the effective radius of the BCG) from the cluster center the surface mass density profile of the total mass and global (cluster plus substructures) dark-matter are steeper and that of the diffuse (cluster) dark-matter is shallower than a NFW profile. Our current analysis does not point to a significant offset between the cluster stellar and dark-matter components. This detailed and robust reconstruction of the inner dark matter distribution in a larger sample of galaxy clusters will set a new benchmark for different structure formation scenarios.

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A refined mass distribution of the cluster MACS J0416.1−2403 from a new large set of spectroscopic multiply lensed sources

Cited by 134 publications

References 75 publications

The Relationship Between Brightest Cluster Galaxy Star Formation and the Intracluster Medium in CLASH

The Relationship Between Brightest Cluster Galaxy Star Formation and the Intracluster Medium in CLASH

Mass distribution in the core of MACS J1206

Mass Profile Decomposition of the Frontier Fields Cluster MACS J0416-2403: Insights on the Dark-matter Inner Profile

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