Small-scale Feedback Research Articles

DUVET: Resolved direct metallicity measurements in the outflow of starburst galaxy NGC 1569

Abstract We present the results of direct-method metallicity measurements in the disk and outflow of the low-metallicity starburst galaxy NGC 1569. We use Keck Cosmic Web Imager observations to map the galaxy across 54″ (800 pc) along the major axis and 48″ (700 pc) along the minor axis with a spatial resolution of 1″ (∼15 pc). We detect common strong emission lines ([O iii] λ5007, Hβ, [O ii] λ3727) and the fainter [O iii] λ4363 auroral line, which allows us to measure electron temperature (Te) and metallicity. Theory suggests that outflows drive metals out of the disk driving observed trends between stellar mass and gas-phase metallicity. Our main result is that the metallicity in the outflow is similar to that of the disk, Zout/ZISM ≈ 1. This is consistent with previous absorption line studies in higher mass galaxies. Assumption of a mass-loading factor of $\dot{M}_{\rm out}/{\rm SFR}\sim 3$ makes the metal-loading of NGC 1569 consistent with expectations derived from the mass-metallicity relationship. Our high spatial resolution metallicity maps reveal a region around a supermassive star cluster (SSC-B) with distinctly higher metallicity and higher electron density, compared to the disk. Given the known properties of SSC-B the higher metallicity and density of this region are likely the result of star formation-driven feedback acting on the local scale. Overall, our results are consistent with the picture in which metal-enriched winds pollute the circumgalactic medium surrounding galaxies, and thus connect the small-scale feedback processes to large-scale properties of galaxy halos.

P 22 Effects of multisensory feedback on tremor severity in essential tremor

Introduction : Essential tremor (ET) amplitude is modulated by visual feedback during target-driven movements: In a grip force task, tremor amplitude increases during large-scale visual feedback compared to low-scale visual feedback. It has not been examined whether visual feedback exclusively modulates action tremor severity or if an increase of other afferent input like auditory information has a modulatory effect on tremor amplitude as well. Also, it is unknown whether the sensory signal itself directly affects the tremor generating network or if the effect is rather indirect: enhanced sensory feedback during targeted driven movements might cause arousal/psychological stress. We hypothesized that (1) amplitude of ET is modulated by variation of auditory feedback in the absence of visual feedback in a force tremor paradigm; (2) increase of tremor amplitude coincides with pupillary dilation as a measure of arousal / psychological stress, independently of the quality of sensory feedback Patients & Methods : 14 ET patients conducted a computer-based experiment in which they were asked to match a target force in a force sensor using their thumb and index finger. The quality of them matching the target force was fed back to the participant visually, auditory or a combination of both. For the visual feedback, 2 bars were displayed on a screen, with the distance between these bars decreasing with approximation of the target force. In auditory feedback, a target tone of 440Hz was asked to match by a second tone which changed pitch when approximating the target force. The amplitude of feedback was manipulated via a scaling factor resulting in a large scale and a small scale feedback condition. To characterize the performance (RMSE to target force) and the tremor severity (Power 4-12 Hz) a 3x2 ANOVA was conducted. To control for arousal / psychological stress-induced via the task, pupillometry was recorded. Results : First results showed a comparable deviation from the target force (RMSE) during the experiment in all three sensory feedback modalities. Additionally, tremor severity did not differ between sensory feedback modalities. The ANOVA revealed an effect of the scaling factor on the tremor severity (Power 4-12Hz) for the visual and also for the auditory feedback condition. Pupillometry consistently showed a significantly increased pupil diameter during the large-scale visual- and auditory feedback conditions compared to the small-scale feedback conditions. Conclusion : Our preliminary findings suggest that action tremor in ET is firstly modulated not only by visual but also auditory feedback in a comparable manner and seems to be modality independent. Secondly, arousal / cognitive stress, as measured here by the pupil size, could mediate the increase of tremor amplitude. Further work is required better understand the role of these two possible mechanisms underlying target-related tremor.

Star-forming regions at the periphery of the supershell surrounding the Cyg OB1 association - II. ISM kinematics and YSOs in the star cluster vdB 130 region

ABSTRACT We present an observational study of small-scale feedback processes operating in the star-forming region located in the wall of the expanding supershell around the Cyg OB1 association. The interstellar gas and dust content and pre-stellar populations in the vicinity of the open star cluster vdB 130 are analysed based on new optical and IR observations performed with the 6-m (3D spectroscopic mapping in the [S ii] doublet) and 2.5-m (optical and NIR images) Russian telescopes along with the archival data of Spitzer and Herschel space telescopes. Analysing ionized gas kinematics and emission spectra, we discovered a compact region with supersonic motions. These motions may be caused either by stellar wind or a bipolar outflow from a protostellar disc. Young stellar objects were identified and classified in the area under study. Two star-forming regions were identified. One of them is a region of ongoing star formation in the head of the molecular cloud observed there and another one is a burst of star formation in the cloud tail.

MODELING HOT GAS FLOW IN THE LOW-LUMINOSITY ACTIVE GALACTIC NUCLEUS OF NGC 3115

Based on the dynamical black hole (BH) mass estimates, NGC3115 hosts the closest billion solar mass BH. Deep studies of the center revealed a very underluminous active galactic nucleus (AGN) immersed in an old massive nuclear star cluster. Recent $1$~Ms \textit{Chandra} X-ray visionary project observations of the NGC3115 nucleus resolved hot tenuous gas, which fuels the AGN. In this paper we connect the processes in the nuclear star cluster with the feeding of the supermassive BH. We model the hot gas flow sustained by the injection of matter and energy from the stars and supernova explosions. We incorporate electron heat conduction as the small-scale feedback mechanism, the gravitational pull of the stellar mass, cooling, and Coulomb collisions. Fitting simulated X-ray emission to the spatially and spectrally resolved observed data, we find the best-fitting solutions with $\chi^2/dof=1.00$ for $dof=236$ both with and without conduction. The radial modeling favors a low BH mass $<1.3\times10^{9}M_\odot$. The best-fitting supernova rate and the best-fitting mass injection rate are consistent with their expected values. The stagnation point is at $r_{\rm st}\lesssim1$arcsec, so that most of gas, including the gas at a Bondi radius $r_B=2-4$arcsec, outflows from the region. We put an upper limit on the accretion rate at $2\times10^{-3}M_\odot{\rm yr}^{-1}$. We find a shallow density profile $n\propto r^{-\beta}$ with $\beta\approx1$ over a large dynamic range. This density profile is determined in the feeding region $0.5-10$arcsec as an interplay of four processes and effects: (1) the radius-dependent mass injection, (2) the effect of the galactic gravitational potential, (3) the accretion flow onset at $r\lesssim1$arcsec, and (4) the outflow at $r\gtrsim1$arcsec. The gas temperature is close to the virial temperature $T_v$ at any radius.

Characterization of periodic flow structure in a small-scale feedback fluidic oscillator under low-Reynolds-number water flow

Numerical simulation and experimentation using high time-resolved particle imaging velocimetry were conducted in order to clarify the flow characteristics in a small-scale feedback fluidic oscillator operated under low-Reynolds-number water flow. Flow oscillations were triggered by the Coanda effect and a periodically oscillating jet. Based on spectral analysis of the velocity fluctuations inside the oscillator body, the Strouhal number was not constant and the frequency was not linear with respect to the flow rate for the Reynolds number range from 238 to 714. The flow rate fluctuations of the feedback flows through the two feedback channels were determined quantitatively. By comparing the simulation and experimental results, the mechanism of the small-scale feedback fluidic oscillator was clarified by considering the time for a jet to oscillate from the center of the control region to either of the attachment walls and the time for a jet to oscillate from either of the attachment walls to the center of the control region separately.

Feeding and Small-scale Feedback in Low-Luminosity AGNs

AbstractThe unmatched X-ray resolution of Chandra allows probing the gas flow near quiescent supermassive black holes (BHs). The radius of BH gravitational influence on gas, called the Bondi radius, is resolved in Sgr A* and NGC 3115. Shallow accretion flow density profiles n ∝ r−β with β=0.7–1.0 were found for Sgr A* and NGC 3115 with the help of Chandra. We construct self-consistent models with gas feeding and dynamics from near the Bondi radius to the event horizon to explain the observations. Gas is mainly supplied to the region by hot colliding stellar winds. Small-scale feedback such as conduction effectively flattens the density profile from steep β=1.5 in a Bondi flow. We further constrain density and temperature profiles using the observed radio/sub-mm radiation emitted near the event horizon. We discuss the present state of our numerical model and its qualitative features, such as the role of the galactic gravitational potential and the random motion of wind-emitting stars.

Large– and small–scale feedback in the Starburst centers of galaxies

The interplay between stellar populations and gas in local starburst galaxies is analyzed using images from the Hubble Space Telescope to map the ages of the young stellar components and to isolate the contribution of shocks on spatial scales ranging from a few tens of pc to ∼1 kpc. The shocked gas represents a small fraction of the total ionized gas in these objects, yet it can have profound effects on the long–term evolution of the starburst, which may include the triggering of new star formation. To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The Ionized Gas in Local Starburst Galaxies: Global and Small-Scale Feedback from Star Formation

Abridged: The small-- and intermediate--scale structure and the fraction of the ISM ionized by non--radiative processes is investigated in a small sample of four local starburst galaxies, imaged with the HST WFPC2. The sample comprises three dwarf galaxies, NGC3077, NGC4214, and NGC5253, and one giant spiral, NGC5236 (M83). The galaxies span a range in metallicity, luminosity, and environment, enabling the investigation of non--radiative ionization processes in a variety of galactic conditions. For this purpose, the four galaxies were imaged in the lines of H-beta(4861 A), [OIII](5007 A), H-alpha(6563 A), and [SII](6717,6731 A). The non--photoionized gas in these galaxies has been traced on scales ranging from a few tens of pc to a few hundred pc, providing a full budget for this ionized gas component. Using the `maximum starburst line' of Kewley et al. (2001) to discriminate between photoionized and non--photoionized gas, we find that in all four galaxies non--photoionization processes are responsible for a small fraction of the total H-alpha emission, at the level of 3%--4%. The starbursts in the three dwarf galaxies deposit a significant fraction, 70%-100%, of their mechanical energy into the surrounding interstellar medium and require time--extended (a few x 10^7 yr to ~10^8 yr) star formation, in order to account for the observed luminosity of the non--photoionized gas. In the massive spiral, the non--photoionized gas is concentrated in localized areas surrounded by active star--formation, with no evidence for extended structures (as those in the dwarfs). This confirms the picture that starbursts remain confined events in massive galaxies, likely due to the deep potential well.