Multi-Scale
Star Formation

April, 3-7th 2017
Morelia, Michoacán. México

Deadlines:


Dinner and Tour reservation: March 10th 2017

Early registration: January 31st 2017

Abstract submission: December 2nd 2016

Rationale

Our understanding of the physical and chemical processes that culminate in the formation of stars and stellar clusters in the Universe has undergone great progress in recent years, both from observations and from theory and simulations. One of the main realizations is that the star-formation process involves a continuous gas flow from galactic (kpc) scales down to stellar (AU) scales. However, there is still a lack of exchange from the different communities performing research in this topic at different characteristic scales.

Given the need to cross-link processes over this wide range of scales, this conference aims at bringing together experts that work in all the relevant scales related to star formation, with the hope that researchers working in a given scale range will bring in their point of view to workers at other scales, improving our understanding of star formation as a broader theme. To achieve this, each session will contain contributed talks from different scales, although preserving an underlying scheme. The invited talks will seek to relate a specific topic to the broader context. There will also be time allocated for two or three one-hour discussion sessions to exchange ideas on the relation of a specific scale to the others.

Venue

The conference will be held at the University Cultural Center (Centro Cultural Universitario) of the "Universidad Michoacana de San Nicolás de Hidalgo" (UMSNH). This is a beautiful colonial-style building with an auditorium for 300 people and several smaller meeting rooms, located at the heart of downtown Morelia, within 2 blocks of the Cathedral, and within walking-distance from several hotels. For more information, click on the following link:

http://www.mexicoescultura.com/recinto/55277/en

The city of Morelia is the capital of the state of Michoacán in central México. Before the spanish colonization, the area was inhabited by the purépecha and the matlatzinca cultures, but no major cities were founded in the valley during this time. The spanish founded a settlement here in 1541 with the name of Valladolid. After the mexican war of independence, the city was renamed Morelia in honor of José María Morelos, one of the main leaders of the war. Morelia is currently a beautiful colonial city, with an ordinance that no building should be taller than its cathedral's towers, to preserve its majestic dominance over the landscape. Morelia was declared a UNESCO World Heritage Site in 1991.

For more information about Michoacán, please visit the site Visit Michoacan (spanish only). Or download the Travel Guide (English/Spanish).

Travel

Taxi Sharing

Dear participants, in the following google document you will be able to share a taxi or take a place of one already shared.

By plane

Morelia is served by General Francisco Mújica international airport (MLM) which is located at the edge of town. Going to the city center takes about half an hour. Book the taxi within the terminal (in “Taxi autorizado”) and take the ticket to the taxi area (~400 MXN or ~20 USD). There are daily international flights from Los Angeles, Dallas-Fort Worth, Houston, and Chicago-Midway which lead to Morelia's international airport, as do commuter flights from Guadalajara, Mexico City, Monterrey, and Tijuana.

Arriving to Mexico City airport and then by bus to Morelia
Mexico City has 4 large bus stations (one for each cardinal direction). The best one to come to Morelia is the westward one ("Terminal Poniente", also called "Observatorio"). There, the Autovias and ETN lines depart to Morelia each half an hour or so. ETN is a bit more expensive and more comfortable, but both are OK. Several buses come from the north bus station as well, but much more sparse schedule.

For more information about buses schedule you can visit the buses web site:

To take the taxi from Mexico City airport to the bus station, pay the ticket in one of the authorized booths inside the terminal. There are several booths: one in baggage claim, one just outside customs, and another one just before the exit where the taxis wait. In the booth there are several brands of taxis. Yellow Cab and Nueva Imagen usually have the most cars available at a given time.

Once in Morelia bus station, there is a taxi booth just when you come out to the main hall. Unlike in Mexico City airport, the booth person here most likely will not speak English, so a print-out of your hotel reservation address would help a lot if you don't speak Spanish.

Arriving directly to Morelia airport
There is booth for authorized taxis just outside customs. Probably the booth person and the driver will know some English, but a print-out of your Hotel reservation with address will be helpful. They may ask you if you want to go by the free or the toll highway. The toll-highway route is about 20 min faster and more comfortable. The price difference is about 3 to 5 USD.

By bus

Deluxe buses serve Morelia from all parts of the country, and Morelia's state-of-the-art bus station, located in the north-western part of the city. The bus station consists of separate terminals for first-class and second-class buses. ETN and Autovias bus companies are suggested. It is easy to reach Morelia from either Mexico City or Guadalajara. The bus trip from Guadalajara is about 3-1/2 hours. From Mexico City the trip is around 4 hours. They are services every 15-30 minutes and they leave Mexico City from bus terminal “Poniente” (also known as “Observatorio”). Single tickets cost ~500 pesos (~26 USD).

Moving around

The conference auditorium is located at the city center. Suggested hotels and restaurants are all at walking distances. Buses, “combis” (small vans) and taxis are Morelia’s main means of public transportation. Combis are a good way to see the smaller roads and backstreets of the city. Various destinations are usually indicated on the windshield of these mini-vans. A ride within the city costs ~10 MXN (~0.5 USD). Get in, grab a handle and sit down before the driver speeds up, and then give your money directly to the driver, or to someone else to pass it to the driver for you (you can ask the person “Si no le molesta, por favor”, basically: “Please, if you don’t mind”). Above your head you will find a buzzer to get out at the next corner, or you can simply ask “en la próxima esquina, por favor” (“next corner please”). Taxis are also plentiful and inexpensive (less than 100 MXN or ~5 USD), operating on zone fares. As elsewhere in Mexico, make sure to determine the price before getting into the taxi. Driving in the city is not easy, but with patience you can. Driving in and around Morelia differs little from driving in any urban area. However, there is an “uno y uno” protocol in place. Drivers are actually quite respectful and obey this “one and one” rule, where at an intersection, fall into line, with one vehicle at a time from each direction driving through the intersection. Please be aware that the “centro histórico” (downtown) area rarely has any avaiable parking spaces, but there are several parking lots in the area.

Visa

Some participants may require a visa in order to enter Mexico. Official information of the countries for which a visa is required is available in the following link (Spanish only):

http://www.inm.gob.mx/gobmx/word/index.php/paises-requieren-visa-para-mexico/

If you happen to require a visa, please contact the LOC for assistance.

Accomodation

We provide a map with some of the hotels in the downtown Morelia area, together with the location of the conference venue, on the conference website. Participants should contact hotels directly to arrange for accommodations. Since many of these are located in historic buildings, not all rooms are provided with in-room wi-fi and/or A/C, even in high-end hotels. If either of these is important to you, please check with the hotel at the time of making your reservation. The weather in Morelia in early April is warm and dry, with highs ~ 28 C (82 F) and lows ~ 13 C (55 F).

Two hotels offer special rates for conference participants. To obtain the special rate it is necessary to make the reservation by email or telephone mentioning the code MSSF17. Not applicable for online reservations.
Hotel Misión Catedral (ventascatedralmorelia@hotelesmision.com.mx)
Hotel Alameda (lcchora@hotel-alameda.com.mx)

Restaurants

We provide a list of restaurants in downtown of city, some of them offering vegetarian options (**)

Registration

We will have limited availability of funds for assisting students and young postdocs cover their lodging expenses in Morelia. Interested persons should indicate so at the time of full registration.

Abstract Submission


Participants

Program

Download Program PDF
Download Abstracts PDF
WARNING: This is not a final version of the Program/Abstracts book.
Please consider download again a new version of the PDF during the event.

Posters

The poster dimensions should not exceed the A0 format (118 by 84 cm, or 46.8 by 33.1 in) in portrait mode.

Posters will be assigned a code depending on range of scales: large (L), medium (M), small (S); and a number, such as in S20. The final poster program will be posted here soon, as well as an option to upload it in case the author desires to give a 1 minute presentation of it.

Small Scales

CODE AUTHOR TITLE
PS01 Isequilla, N Radio observations of evaporating in the Cygnus OB2 region
PS02 Gómez Maqueo Chew, YFundamental properties of the eclipsing pre-main sequence components of MML 53
PS03 Koutoulaki, M AMBER/VLTI Medium spectral resolution observations of the Bracket gamma and high-n Pfund emitting regions of the Herbig B[e] star HD50138
PS04 Shan, YMultiplicity of Pre-Main Sequence M-dwarfs in Young Moving Groups (YMGs)
PS05 Guszejnov, DConsequences of Scale Free Fragmentation in Star Formation
PS06 Masqué, JSearching for compact radio sources associated to UCHII regions
PS07 Paron, SMulti-scale and multi-wavelength study of the UCHII G45.47+0.05 surroundings
PS08 Kee, NThe Role of Line-Driven Outflows in the Formation of Massive Protostars
PS09 Sanna, AGas dynamics driven by an O-type YSO: from 0.1 pc down to 100 AU
PS10 Sánchez-Monge, AAn ALMA view of SgrB2: continuum characterization and spectral line survey
PS11 Cappa, CStar formation, gas and dust in the IR dust bubbles complex S21-S24
PS12 Fedriani, RKinematical and Dynamical Study of IRAS 13481-6124 primary jet
PS13 Ahmadi, ACORE: A NOEMA large program to investigate fragmentation and disk kinematics during high-mass star formation
PS14 Ortega, MMisaligned molecular outflows and precessing jet towards the massive young stellar object G034.5964-01.0292
PS15 Kumar, NO-star binary systems in formation
PS16 Hernández, JA large scale survey of Herbig Ae/Be stars in the Orion Star Forming Complex - GAIA view
PS17 Frimann, SLarge-scale numerical simulations of star formation put to the test. Comparing synthetic images and actual observations for statistical samples of protostars.
PS18 Camacho, VEnergy budget of forming clumps in numerical simulations of collapsing clouds
PS19 Feddersen, JProbing a molecular cloud from 0.01 to 10 pc scales: The CARMA Orion Survey
PS20 Sandell, GSOFIA, a unique observatory for studying star formation process
PS21 Sandell, GNGC7538 IRS1 & South – our key to understanding high mass star formation
PS22 Rodríguez-Kamenetzky, ANon-Thermal Emission From Protostellar Jets
PS23 Hernández-Gómez, AVLA centimetric observations towards IRAS16293-2422
PS24 Gómez-Ruiz, APolarization structure of protostellar shocks
PS25 Nony, THigh-mass star formation in the W43-MM1 protocluster
PS26 Sierra, ADust emission of protoplanetary disks
PS27 Suárez, GTowards a complete study of the initial mass function and early kinematics evolution of the 25 Orionis stellar group
PS28 Kölligan, AJets and Outflows of Massive Protostars
PS29 Manzo-Martínez, EEvolutionary models of accretion disks: IR emission and snowlines evolution
PS30 Lopez-Vázquez, AAngular momentum in bipolar outflows
PS31 Sewilo, MThe Very Large Array ammonia observations of the HH 111/HH 121 protostellar system: a detection of a new source with a peculiar chemistry
PS32 Treviño-MoralesDeuteration around the ultracompact HII region Mon R2
PS33 Liao, L.-W.A bipolar molecular jet in NGC2023 MM1
PS34 Rojas, SSearching for collimated outflows candidates in massive star-forming regions
PS35 Tapia, MA new infrared view of the NGC 6634-V region
PS36 Tapia-Schiavón, LThe heating efficiency and the star formation rate in very young stellar clusters
PS37 Ferrero, LSouthern hemisphere jets and molecular outflows observed with Gemini and APEX: the case of HH 137 and HH 138
PS38 Rodríguez-Garza, CA survey of 44-GHz Class I methanol masers toward High Mass Protostellar Objects
PS39 Rodríguez-Garza, CEarly science with the Large Millimeter Telescope: a 3 mm spectral line survey of massive protostars with class I methanol masers
PS40 Ramírez, VKinematics of Cromospherically Active Stars in the RAVE Catalog
PS41 Naranjo-Romero, RHierarchical gravitational fragmentation. I. Collapsing cores within collapsing clouds
PS42 Orozco, TMolecular study of two inter-mediate mass hot cores in OMC1
PS43 Rangaswamy, DNear-Infrared Polarimetry of the S235 star-forming complex
PS44 Zamora, M The magnetic field as a turbulence suppressor in molecular cloud formation
PS45 Toalá, JA young Hot Bubble within the HII region SMC-N88
PS46 Rodgers-Lee, DLow energy protostellar cosmic rays in protoplanetary disks
PS47 Zepeda, DLMT study of 1.1mm cores in Orion A molecular cloud
PS48 Slepian, ZCollapse of spherical cores embedded in a low-density filament: analytic predictions
PS49 Jung, MFirst light emerging from the clouds
PS50 Zhang, HanConstraining the magnetic fields in Young Stellar Objects (YSOs)
PS51 Binks, AImproving ages for nearby, young moving groups
PS52 Lee, Y
PS53 Castañeda, H
PS54 Luna, A

Medium Scales

CODE AUTHOR TITLE
PM01 Barnes, AStar formation rates and efficiencies in the Galactic Centre
PM02 Ramón-Fox, GExploring the role of large scale flows in molecular cloud formation in spiral galaxies
PM03 Dzib, SThe GLOSTAR VLA Galactic plane survey
PM04 Rugel, MOH gas properties and feedback in the Milky Way as seen in the THOR survey
PM05 Medina, STurbulence Analysis on Galactic Plane Molecular Clouds
PM06 Armentrout, WStar Formation Efficiency in the Outer Scutum-Centaurus Arm
PM07 Kendrew, STracing massive stellar feedback in the Milky Way Galaxy
PM08 Colombo, DBuilding a (fully resolved) molecular cloud catalog of the Milky Way
PM09 Fissel, LMagnetic Fields in Star Formation: A Detailed BLASTPol Study of the Vela C Giant Molecular Cloud
PM10 de la Fuente, DEarly evolution of stellar populations in a giant star-forming complex: the Dragonfish nebula
PM11 Hernández, AudraA Catalog of the Southern Molecular Cloud Physical Properties from the ThrUMMS Survey
PM12 Anderson, LThe Galactic Distribution of High-Mass Star Formation Regions
PM13 Rendón, JInsufficient Reservoirs of Molecular Gas to Form a Second Stellar Population in LMC Massive Star Clusters
PM14 Rodríguez, JimenaSystematic study of young star clusters in the galaxy NGC 253
PM15 Smilgys, RFormation of stellar clusters in galactic spiral arms
PM16 Pitts, RContinuum Emission Diagnostics for Pretsellar Clumps in the CHaMP Survey
PM17 Towner, AMid-IR and Centimeter Observations of 20 High-Mass Protoclusters in the Milky Way
PM18 Alzate, JStellar population parameters of the Milky Way Galaxy and photometric detection of satellite galaxy remnants
PM19 Lucas, PHighly variable protostars from the UKIDSS Galactic Plane Survey
PM20 Vavrek, RboloSource() for the analysis of diffuse emission and crowded-field photometry
PM21 Peñaloza, CUsing synthetic observations to constrain the evolution high tracers in molecular clouds

Large Scales

CODE AUTHOR TITLE
PL01 Vega-Acevedo, IStar formation efficiency in tidal tails of mergers
PL02 Pellegrini, EBeyond the Peak Spatially resolved CO Excitation in the Local Universe
PL03 Méndez-Hernández, HProbing the circum-galactic gas with VUDS
PL04 Obi, IkechukwuSEDs of nearby star-forming galaxies with the new PARSEC evolutionary tracks: Star formation rates and Dust Attenuation Properties
PL05 Esparza-Arredondo, DCoevolution between multiscale star-formation and AGN activity
PL06 Hidalgo-Gámez, AThe SFR of compact, coloured galaxies
PL07 Magaña-Serrano, MCalibrando la tasa de formación estelar en Hα y FUV para galaxias tardías
PL08 Ramírez-Siordia, VDeriving the Star Formation History of Stellar Systems Containing Few Stars
PL09 Elías-Chávez, MEstimation of the star formation rate through data analysis of SWIFT's long GRBs from 2008 to 2016
PL10 Calvi, RThe morphological dependences of SFR-mass relations for local star-forming galaxies in different environments star-forming galaxies in different environments
PL11 López-Cobá, CStar-formation driven galactic winds in UGC 10043
PL12 González-Samaniego, AStar formation and mass estimators in dwarfs galaxies vs. cosmological simulations
PL13 Arrabal Haro, PHigh-z Ly_alpha sources search using the SHARDS survey
PL14 Boquien, M
PL15 Hart, R
PL16 Pappalardo, C

SOC

Gustavo Bruzual
Paola Caselli
Francoise Combes
Bruce Elmegreen
Neal Evans
Lee Hartmann
Melvin Hoare
Susana Lizano
Mordecai Mac Low
Frederique Motte
Casiana Munoz Tunon
Luis Felipe Rodriguez
Meg Urry
Enrique Vazquez-Semadeni (chair)
Qizhou Zhang

LOC

Leonardo Arroyo
Roberto Galvan-Madrid
Gilberto Gomez
Omaira Gonzalez-Martin
Ezequiel Manzo
Enrique Vazquez-Semadeni