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Measuring the Logarithmic Spiral-arm Pitch Angle of Spiral Galaxies

Multicomponent Decomposition of Galaxies

Black Hole Mass Scaling Relations

What Causes Spiral Structure in Galaxies?

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Lunar Eclipse – May 15, 2022 – taken with an iPhone SE (2nd Generation), looking through a 6-inch telescope.

Lunar Eclipse – November 19, 2021 – taken with an iPhone SE (2nd Generation), looking through a 6-inch telescope.

Jupiter/Saturn Conjunction – December 21, 2020 – taken with an iPhone SE (2nd Generation), looking through a 6-inch telescope.

Images of face-on spiral galaxies, taken during the nights of November 8-10, 2013, on the 3.5m WIYN telescope.

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"Ben" (2021), portrait by Amanda Cockerham.

Image by James Josephides. Featured in our 2017 Press Release and on the cover of the 2019 Swinburne Annual Report (with a description in the inside cover). LinkedIn post from Alister Graham. Mention on Alister Graham's website.

Measuring the Logarithmic Spiral-arm Pitch Angle of Spiral Galaxies

Spiral galaxies are distinguished by their prominent bright spiral arms. Logarithmic spirals best describe the geometry of their winding. Logarithmic spirals form a continuum of shapes from spirals that are so tightly wound they become circles, to spirals that are so loosely wound that they form straight lines (see the animated gif below). In the animation, the only parameter changing is the "pitch angle" of the spiral pattern. We denote pitch angle with the Greek letter \(\phi\). In general terms, \(\phi\) is the angle between a line tangent to a logarithmic spiral and a line tangent to a circle of radius \(r\) that are constructed from and intersect both at \((r,\theta)\), the reference point (see Figure 1). In equation form, \(\cot\phi=rd\theta/dr\). Tightly wound spirals have low values (down to \(0^\circ)\) of \(\phi\) and loosely wound spirals have high values (up to \(90^\circ)\) of \(\phi\). I use advanced software packages that I helped develop to measure pitch angles of spiral galaxies to quantitatively classify them according to the geometry of their arm winding. These different software routines employ 2D fast Fourier transform (Davis et al. 2012), computer vision (Davis & Hayes 2014), and template fitting (Shields et al. 2022) algorithms. For further details, see Davis et al. (2017), and references therein. Figure A1 overlays the measured spiral arcs on top of the galaxy UGC 6093, demonstrating a mean pitch angle of \(|\phi|\approx10^\circ\pm2^\circ\).

The above animation shows a two-arm logarithmic spiral pattern that begins with \(|\phi|=5^\circ\) and incrementally increases \(|\phi|\) by \(5^\circ\) in each successive frame until \(|\phi|=85^\circ\), then the animation repeats.

Multicomponent Decomposition of Galaxies

Spiral galaxies are composed of many separate major constituents. These can include: (i) a bright point source resulting from a nuclear star cluster or active galactic nucleus, (ii) a bulge or spheroid, (iii) an elongated bar, (iv) rings, (v) ansae (handle-like structures at the end of a bar), (vi) boxy-peanut shaped structures, (vii) exponential disks, which can also be broken (truncated or anti-truncated), (viii) spiral arms, (ix) halos, etc. It is, therefore, possible to analyze the total light of a galaxy and decompose the light profile of a galaxy into its separate components. In the below figures, I demonstrate this accounting of components by showing radial surface brightness profiles of the galaxy UGC 6093. As shown in Figure 54, the galaxy is best described by modeling it with nine components: (1) a central point source (lime green), (2) excess nuclear light (cyan), (3) a bulge (red), (4) a bar (orange), (5) an exponential disk (blue), (6-9) an four radial crossings of spiral arms (cyan). Figure 55 shows the original image of UGC 6093, the model image, residual image, and an annotated image of the modeled components from Figure 54. The whole process detailed in these two figures requires significant image processing and many sophisticated software routines. For full details, Davis et al. (2019), and references therein.

Black Hole Mass Scaling Relations

Supermassive black holes (SMBHs; \(M_{\rm BH}\geq10^5M_\odot\)) are believed to lie at the centers of nearly all galaxies. It is also abundantly evident that SMBHs and their host galaxies must co-evolve. However, our knowledge of this coevolution is perplexed by an analogous "chicken-and-egg" problem: which came first, the black hole or the galaxy? Did the galaxy form, spawn a black hole which subsequently grew and settled in the nucleus of its galaxy, or did the black hole form first and then seeds the growth of an entire galaxy around it? The answer to this fundamental question is important for our understanding of galaxy evolution. Black holes are by nature invisible, and therefore extremely difficult to study and measure. As of 2019, astronomers have only managed to directly measure the masses of 154 black holes in the center of galaxies. From these measurements, we have shown that black hole mass correlates with numerous properties of galaxies, including bulge mass and its light concentration (Davis et al. 2019); disk and total mass (Davis et al. 2018); the shear parameter of the galactic rotation curve (Seigar et al. 2014); the maximum rotational velocity of the disk and dark matter halo mass (Davis et al. 2019); stellar velocity dispersion of the bulge (Davis et al. 2017); etc. See also Sahu et al. (2019a), Sahu et al. (2019b), Sahu et al. (2020), Sahu et al. (2022a), Sahu et al. (2022b), and Davis & Jin (2023).

However, perhaps the most surprising result is the strong correlation between the geometry of spiral arms (i.e., logarithmic spiral-arm pitch angle) in spiral galaxies and their central black holes' mass (see Berrier et al. 2013; Davis et al. 2017, and references therein). Specifically, spiral galaxies with more tightly wound spiral arms possess more massive black holes and vice versa (see the figure below from Davis & Graham 2021). Thus, measuring the structure of spiral galaxies is a powerful tool for estimating the mass of black holes in galaxies by only measuring pitch angle, which only requires simple imaging and does not require complicated spectrographic studies. By combining all of the aforementioned scaling relations, we can use multiple independent methods to identify galaxies that could potentially harbor elusive intermediate-mass black holes (IMBHs; \(10^2M_\odot\leq M_{\rm BH}<10^5M_\odot\)). IMBHs pose a gaping missing link in the evolutionary demographics of black holes because both smaller solar mass black holes (\(M_{\rm BH}<10^2M_\odot\)) and larger SMBHs have been directly detected. Therefore, identifying candidate galaxies that could warrant follow-up studies and possible confirmation of IMBHs is an essential endeavor in the field of black holes (Koliopanos et al. 2016; Graham et al. 2019; Graham et al. 2021a; Graham et al. 2021b). Finally, by measuring large populations of black holes, we can take a census of black holes in the universe garner information about their demographics (Davis et al. 2014; Mutlu-Pakdil et al. 2016; Fusco et al. 2022).

Spiral galaxy arms with varying degrees of tightness, and the corresponding galaxy type and central black hole mass in units of our Sun’s mass. This template can be used to estimate the black hole masses in spiral galaxies.

Planar black hole mass scaling relation between black hole mass, pitch angle, and maximum rotational velocity (Davis & Jin 2023).

What Causes Spiral Structure in Galaxies?

Spiral structure was first observed in Messier 51a, aka "The Whirlpool" galaxy, by Lord Rosse in 1845. We now know that spiral galaxies make up approximately 60% of galaxies in today's universe. However, astronomers are still perplexed about what mechanism generates and maintains spiral structure in galaxies. Of the numerous theories that have been proposed, perhaps spiral density wave theory is the most intuitive and enduring of the theories. Spiral density wave theory posits quasistatic density waves propagate through the disks of galaxies and triggers spiral-shaped regions of enhanced star formation by locally compressing the gas and triggering enhanced star formation. These quasistatic density waves are akin to traffic jams where individual cars may enter and then leave the location of the traffic jam, but the jam itself remains relatively stationary. This is also representative of a standing wave on a vibrating string, where the nodes of vibration remain fixed. If this acoustic analogy is further explored, we find that the frequency of a vibrating string is also analogous to the pitch angle of a spiral galaxy. For a string of fixed length (like on a string instrument), its frequency is determined by two parameters: (i) the tension in the string and (ii) the density per unit length of the string. Similarly, the pitch angle of winding in a galaxy's spiral pattern (which can be thought of as a frequency of winding) is also determined by two parameters: (i) the central mass of the galaxy and (ii) the density of the galactic disk.

On a violin, tightening a tuning peg increases the tension in a string and increases the frequency that is heard. Comparably, increasing the central mass of a galaxy increases its gravitational attraction, and pulls more strongly on the spiral pattern of the galaxy, making it tighter. Also on a violin, the thicker gauge (denser) strings vibrate with a lower frequency than the thinner gauge (less dense) strings. Likewise, decreasing the density of gas in the disk of a galaxy also speeds up the propagation of the density wave and tightens the winding of the spiral pattern, just as inhaling helium and then speaking increases the frequency of your voice. In Davis et al. (2015), we verified from observations that this three-parameter correlation exists between the central mass of a galaxy, the density of gas in its disk, and the pitch angle of its spiral pattern (see Figure 1 below). Furthermore, Pour-Imani et al. (2016) confirmed the prediction of spiral density wave theory that the spiral pattern should appear slightly different when observed in different wavelengths of light. We studied 41 spiral galaxies in various wavelengths of light, ranging from far-ultraviolet to near-infrared (see also Miller et al. 2019). We found that spiral patterns are slightly looser when the filter of light highlights blue, young star-forming regions and is marginally tighter when the filter highlights red, old stellar populations. This is evidence that stars which form the spiral pattern are born in the density wave and then drift out of the density wave, just like cars emerging from a traffic jam (see Figure 2 below). For additional studies, see Abdeen et al. 2020 and Miller et al. 2022.

Figure 1. Three-dimensional plot of the plane depicted by a translucent blue meshed surface, along with the plotted points of the 24 galaxy member included data set (depicted by red spheres with the Milky Way in green). The axes \([x, y, z]\) depict \([\tan|P|\), \(\log(M_{\star}^{bulge}/M_{\odot})\), \(\Sigma_{H_{I}}^{max}]\), respectively.

Figure 2. Predictions of density-wave theory for spiral-arm structure with old stars, blue stars, gas, and dust. On the left is a scenario where star formation occurs after gas clouds pass through the minimum of the potential of the density wave. On the right is a scenario in which star formation occurs as the gas clouds approach this minimum of the potential.