The<i>Spitzer</i>Survey of Stellar Structure in Galaxies

Sheth, Kartik; Regan, Michael W.; Hinz, J. L.; Paz, A. Gil de; Menéndez‐Delmestre, Karín; Muñoz-Mateos, J. C.; Seibert, Mark; Kim, Tae Hyun; Laurikainen, Eija; Salo, H.; Gadotti, Dimitri A.; Laine, Jarkko; Mizusawa, Trisha; Armus, L.; Athanassoula, E.; Bosma, A.; Buta, Ronald J.; Capak, P.; Jarrett, T. H.; Elmegreen, D. M.; Elmegreen, Bruce G.; Knapen, Johan H.; Koda, Jin; Hélou, G.; Ho, Luis C.; Madore, Barry F.; Masters, Karen L.; Mobasher, Bahram; Ogle, Patrick; Peng, Chien Y.; Schinnerer, E.; Surace, J.; Zaritsky, Dennis; Comerón, Sébastien; Swardt, Bonita de; Meidt, Sharon E.; Kasliwal, M. M.; Aravena, M.

doi:10.1086/657638

Cited by 517 publications

(534 citation statements)

References 115 publications

Supporting

Mentioning

501

Contrasting

Order By: Relevance

“…Our galaxies are large and nearby, which allows us to perform accurate multicomponent decompositions (instead of simple bulge/disk decompositions). Our decompositions were performed on 3.6 m m Spitzer satellite imagery, which is an excellent proxy for the stellar mass, superior to the K-band (Sheth et al 2010, and references therein). Nine of our galaxies have M M 10 , BH 7   which allows us to better constrain the slope of the correlation at the low-mass end.…”

Section: Introductionmentioning

confidence: 99%

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

Savorgnan

Graham

Marconi

et al. 2016

ApJ

130

181

View full text Add to dashboard Cite

In our first paper, we performed a detailed (i.e., bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, M BH , imaged at 3.6 m m with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between M BH and the host spheroid (and galaxy) luminosity, L sph (and L gal ), and also stellar mass, M .,sph * While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have M M 10 , argued by some to be pseudo-bulges, are not offset to lower M BH from the correlation defined by the current bulge sample with n 2; sph > and (3)L sph and L gal correlate equally well with M BH , in terms of intrinsic scatter, only for early-type galaxies-once reasonable numbers of spiral galaxies are included, the correlation with L sph is better than that with L gal .

show abstract

Section: Introductionmentioning

confidence: 99%

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

Savorgnan

Graham

Marconi

et al. 2016

ApJ

130

181

View full text Add to dashboard Cite

show abstract

“…The IRAC 3.6µm images of NGC 4013 and NGC 5529 were downloaded from the Spitzer Survey of Stellar Structure in Galaxies archive 4 (S4G, Sheth et al 2010), along with the masks and weight (one-sigma) images. The sky background has already been subtracted from these frames.…”

Section: Images Preparationmentioning

confidence: 99%

Measuring the X-shaped structures in edge-on galaxies

Савченко

Sotnikova

Mosenkov

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present a detailed photometric study of a sample of 22 edge-on galaxies with clearly visible X-shaped structures. We propose a novel method to derive geometrical parameters of these features, along with the parameters of their host galaxies based on the multi-component photometric decomposition of galactic images. To include the X-shaped structure into our photometric model, we use the IMFIT package, in which we implement a new component describing the X-shaped structure. This method is applied for a sample of galaxies with available SDSS and Spitzer IRAC 3.6 µm observations. In order to explain our results, we perform realistic N -body simulations of a Milky Way-type galaxy and compare the observed and the model X-shaped structures. Our main conclusions are as follows: (1) galaxies with strong Xshaped structures reside in approximately the same local environments as field galaxies; (2) the characteristic size of the X-shaped structures is about 2/3 of the bar size; (3) there is a correlation between the X-shaped structure size and its observed flatness: the larger structures are more flattened; (4) our N -body simulations qualitatively confirm the observational results and support the bar-driven scenario for the X-shaped structure formation.

show abstract

“…We vary the parameters influencing the slope of the inner rotation curve, and show how this affects the face-on morphology of the vertically extended inner bar region. The S 4 G survey (Spitzer Survey of Stellar Structure in Galaxies; Sheth et al 2010) is used as a guide for choosing the simulations parameters, and also as a comparison sample to check the predictions of the simulations.…”

Section: Introductionmentioning

confidence: 99%

Boxy/Peanut/X-shaped Bulges: Steep Inner Rotation Curve Leads to Barlens Face-on Morphology

Salo

Laurikainen

2017

ApJ

View full text Add to dashboard Cite

We use stellar dynamical bulge/disk/halo simulations to study whether barlenses (lens-like structures embedded in the narrow bar component) are only the face-on counterparts of Boxy/Peanut/X-shapes (B/P/X) seen in edge-on bars, or if some additional physical parameter affects that morphology. A range of bulge-to-disk mass and size ratios are explored: our nominal parameters (, disk comprisingtwo-thirds of total force at h 2.2 r ) correspond to typical Milky Way mass galaxies. In all models, a bar with pronounced B/P/X forms in a few Gyr, visiblein the edge-on view. However, the pure barlens morphology forms only in models with sufficiently steep inner rotation curves,, achieved when including a small classical bulge with  B D 0.02 and  r h 0.1 r eff . For shallower slopes, the central structure still resembles a barlens, but shows a clear X signature even in low inclinations. A similar result holds for bulge-less simulations, where the central slope is modified by changing the halo concentration. The predicted sensitivity on the inner rotation curve is consistent with the slopes that are estimated from gravitational potentials calculated from the 3.6 μm images, for the observed barlens and X-shaped galaxies in the Spitzer Survey of Stellar Structure in Galaxies (S 4 G). For inclinations <60°t he galaxies with barlenses have on average twice steeper inner rotation curves than galaxies with X shapes: the limiting slope is ∼250 km s −1 kpc −1 . Among barred galaxies, those with barlenses have both the strongest bars and the largest relative excess of inner surface density, both in barlens regions ( h 0.5 r ) and near the center ( h 0.1 r ); this provides evidence for bar-driven secular evolution in galaxies.

show abstract

TheSpitzerSurvey of Stellar Structure in Galaxies

Cited by 517 publications

References 115 publications

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

Measuring the X-shaped structures in edge-on galaxies

Boxy/Peanut/X-shaped Bulges: Steep Inner Rotation Curve Leads to Barlens Face-on Morphology

Contact Info

Product

Resources

About

TheSpitzerSurvey of Stellar Structure in Galaxies

Cited by 517 publications

References 115 publications

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE MBH–M*,SPH DIAGRAM

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE MBH–M*,SPH DIAGRAM

Measuring the X-shaped structures in edge-on galaxies

Boxy/Peanut/X-shaped Bulges: Steep Inner Rotation Curve Leads to Barlens Face-on Morphology

Contact Info

Product

Resources

About

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM

SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. II. THE RED AND BLUE SEQUENCE IN THE M_BH–M_*,SPH DIAGRAM