An extensive photometric catalogue of CALIFA galaxies

Gilhuly, Colleen; Courteau, Stéphane

doi:10.1093/mnras/sty756

Cited by 16 publications

(27 citation statements)

References 62 publications

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“…In contrast, Neumann et al (2017) and Gilhuly & Courteau (2018) advocated a classical bulge for the galaxy. The 2D decompositions of the SDSS images of NGC 7025 by Neumann et al (2017) and Gilhuly & Courteau (2018) were performed without accounting for the galaxy intermediate (spiral-arm) component (see also Rizzo et al 2018), this biased their Sérsic index and flux for the bulge component towards higher values, which are expected for classical bulges (see Section 3.2.1).…”

Section: The Nature Of the Disky Bulge In Ngc 7025mentioning

confidence: 98%

“…Recently, Neumann et al (2017), Rizzo et al (2018) and Gilhuly & Courteau (2018) fit a 2D Sérsic bulge + exponential disk model to the SDSS images of NGC 7025, without accounting for the intermediate (spiral-arm) component. As warned by Dullo et al (2016Dullo et al ( , 2017Dullo et al ( , 2018, see also Dullo & Graham 2012, 2014Graham et al 2016 Tables 1 and 3).…”

Section: Comparison With Past Decompositionmentioning

confidence: 99%

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High-resolution MEGARA Integral-field Unit Spectroscopy and Structural Analysis of a Fast-rotating, Disky Bulge in NGC 7025

Dullo

Chamorro-Cazorla

Paz

et al. 2019

ApJ

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Disky bulges in spiral galaxies are commonly thought to form out of disk materials (mainly) via bar driven secular processes, they are structurally and dynamically distinct from 'classical bulges' built in violent merger events. We use high-resolution GTC/MEGARA integral-field unit spectroscopic observations of the Sa galaxy NGC 7025, obtained during the MEGARA commissioning run, together with detailed 1D and 2D decompositions of this galaxy's SDSS i-band data to investigate the formation of its disky (bulge) component which makes up ∼ 30% of the total galaxy light. With a Sérsic index n ∼ 1.80 ± 0.24, half-light radius R e ∼ 1.70 ± 0.43 kpc and stellar mass M * ∼ (4.34 ± 1.70) × 10 10 M ⊙ , this bulge dominates the galaxy light distribution in the inner R ∼ 15 ′′ (∼ 4.7 kpc). Measuring the spins (λ) and ellipticities (ǫ) enclosed within nine different circular apertures with radii R ≤ R e , we show that the bulge, which exhibits a spin track of an outwardly rising λ and ǫ, is a fast rotator for all the apertures considered. Our findings suggest that this inner disky component is a pseudo-bulge, consistent with the stellar and dust spiral patterns seen in the galaxy down to the innermost regions but in contrast to the classical bulge interpretation favored in the past. We propose that a secular process involving the tightly wound stellar spiral arms of NGC 7025 may drive gas and stars out of the disk into the inner regions of the galaxy, building up the massive pseudo-bulge.

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Section: The Nature Of the Disky Bulge In Ngc 7025mentioning

confidence: 98%

Section: Comparison With Past Decompositionmentioning

confidence: 99%

High-resolution MEGARA Integral-field Unit Spectroscopy and Structural Analysis of a Fast-rotating, Disky Bulge in NGC 7025

Dullo

Chamorro-Cazorla

Paz

et al. 2019

ApJ

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“…The CALIFA Fundamental Plane, viewed edge-on, generated using Pipe3D V1200 stellar velocity dispersions. R e and µ e are sourced from theGilhuly & Courteau (2018) CALIFA photometry catalog. The dashed line corresponds to the fitted edge-on plane.…”

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confidence: 99%

Pipe3D stellar and gaseous velocity dispersions for CALIFA Galaxies

Gilhuly

Courteau

Sánchez

2018

Monthly Notices of the Royal Astronomical Society

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We present tables of velocity dispersions derived from CALIFA V1200 datacubes using Pipe3D. Four different dispersions are extracted from emission (ionized gas) or absorption (stellar) spectra, with two spatial apertures (5 and 30 ). Stellar and ionized gas dispersions are not interchangeable and we determine their distinguishing features. We also compare these dispersions with literature values and construct sample scaling relations to further assess their applicability. We consider revised velocity-based scaling relations using the virial velocity parameter S 2 K = KV 2 rot + σ 2 constructed with each of our dispersions. Our search for the strongest linear correlation between S K and i-band absolute magnitudes favors the common K ∼ 0.5, though the range 0.3-0.8 is statistically acceptable. The reduction of scatter in our best stellar mass-virial velocity relations over that of a classic luminosity-velocity relation is minimal; this may however reflect the dominance of massive spirals in our sample.

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“…Following (Gao & Ho 2017), we assign 10% fractional uncertainty to B/T . The concentration indices (C 28 ), derived from the isophotal analysis of Gilhuly & Courteau (2018), have fractional errors pf 3%. The absolute B-band magnitudes (M B ) come from HyperLeda (Paturel et al 2003).…”

Section: Datamentioning

confidence: 99%

“…From this original sample, after discarding galaxy mergers and cases with uncertain dynamical models, Kalinova et al (2017) derived circular velocity curves for 238 objects using detailed stellar dynamical Jeans modeling (Cappellari 2008). Other galaxy properties, such as stellar masses, photometric decomposition, and star formation rates are also available (Walcher et al 2014;Sánchez et al , 2017Méndez-Abreu et al 2017;Catalán-Torrecilla et al 2017;Gilhuly & Courteau 2018). This database enables us to perform a comprehensive study of the dependence of spiral arm pitch angle on various galaxy properties.…”

Section: Introductionmentioning

confidence: 99%

On the Connection between Spiral Arm Pitch Angle and Galaxy Properties

2019

ApJ

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We measure the pitch angle (ϕ) of spiral arms in a sample of 79 galaxies to perform a systematic study of the dependence of ϕ on galaxy morphology, mass, and kinematics to investigate the physical origin of spiral arms. We find that ϕ decreases (arms are more tightly wound), albeit with significant scatter, in galaxies with earlier Hubble type, more prominent bulges, higher concentration, and larger total galaxy stellar mass (M gal * ). For a given concentration, galaxies with larger stellar masses tend to have tighter spiral arms, and vice versa. We also find that ϕ obeys a tight inverse correlation with central stellar velocity dispersion for σ c 100 km s −1 , whereas ϕ remains approximately constant for σ c 100 km s −1 . We demonstrate that the ϕ -σ c and ϕ -M gal * relations are projections of a more fundamental three-dimensional ϕ − σ c − M gal * relation, such that pitch angle is determined by σ c for massive galaxies but by M gal * for less massive galaxies. Contrary to previous studies, we find that ϕ correlates only loosely with the galaxy's shear rate. For a given shear rate, spirals generated from Nbody simulations exhibit much higher ϕ than observed, suggesting that galactic disks are dynamically cooler (Toomre's Q ≈ 1.2). Instead, the measured pitch angles show a much stronger relation with morphology of the rotation curve of the central region, such that galaxies with centrally peaked rotation curves have tight arms, while those with slow-rising rotation curves have looser arms. These behaviors are qualitatively consistent with predictions of density wave theory.

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An extensive photometric catalogue of CALIFA galaxies

Cited by 16 publications

References 62 publications

High-resolution MEGARA Integral-field Unit Spectroscopy and Structural Analysis of a Fast-rotating, Disky Bulge in NGC 7025

High-resolution MEGARA Integral-field Unit Spectroscopy and Structural Analysis of a Fast-rotating, Disky Bulge in NGC 7025

Pipe3D stellar and gaseous velocity dispersions for CALIFA Galaxies

On the Connection between Spiral Arm Pitch Angle and Galaxy Properties

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