I am an Astronomer studying transient phenomena associated with the death of massive stars and/or the explosion of white dwarfs. Recently, I have become quite keen to study supernovae discovered in the hours to days after exploding in order to directly measure the radius of the progenitor star and/or that of a companion star.

Early phase studies of supernovae


What are the progenitors of different kinds of supernovae? How do these stars explode? One of the best ways to gain insight into SN progenitors and their explosion physics is with early data in the hours to days after they explode. The early emission from SNe is generally dominated by the explosion itself rather than radioactive decay and can be used to measure the radius of the exploding star (Piro & Nakar 2013), a fundamental property of the explosion. The early light curve can also measure properties of a companion star (Kasen 2010), the presence of which is still an outstanding question for SNe Ia and thought to be critical for generating many stripped-envelope SNe. The rise of the early light curve can measure the outer 56Ni distribution (Piro 2012), an important constraint for explosion models. Furthermore, observations on these timescales can even help us study entirely new classes of transients, including the radioactively powered kilonovae that are expected from neutron star mergers (Metzger et al. 2010) and will be crucial for gravitational wave detections, and the shock breakout expected during black hole formation (Piro 2013), the birth of which have never been observed.

Motivated by the early-time science opportunities described above, through the ASAS-SN project we aim to discovery young, nearby supernovae using a network of robotic telescopes. Currently, my PhD student S. Holmbo is working on a number of supernovae discovered young and observed by the CSP and/or NUTS. This sample includes the Type Ia supernova 2013gy, which was discovered within 1 day of explosion.


Near Field Cosmology

The Carnegie Supernova Project and the Carnegie Supernova Project II overall aim is to obtain the most precise Type Ia supernova distances possible as well as to obtain high-quality light curves and spectroscopy time-series of many varities of supernovae. The CSP I obtained detailed light curves of 130 SN Ia with a sample mean redshift z=0.02. Thereafter the CSP II obtained light curves and spectroscopy of ~250 SNe Ia with the first ever near-IR (NIR) sub-sample characterized by as sample mean redshift of z=0.06. These data sets will serve as a cornerstone to achieve SN Ia luminosities accurate to 1-2% out to significant cosmological distances.




type IaX supernovae

Type IaX supernovae loosely resemble normal Type Ia supernovae though they have distinct differences. I have worked on a large number of Type IaX supernovae. For example, shown in the figure is the first candidate progenitor of a white dwarf system that produced the Type IaX supernova 2012Z. Details on the progenitor detection in pre-explosion HST images are presented in our paper in Nature (McCully et al. 2014, Nature, 512, 54), while comprehensive observations of supernova 2012Z are presented in a companion paper (Stritzinger et al. 2015, A&A, 573, 2), where I argue that at least some of their progenitors are Chandrasekhar-mass white dwarfs exploding via a pulsational delayed-deontation mechanism.
Other individual SNe IaX I have worked on include: SN 2008ge (Foley et al. 2010, AJ, 140, 1321), SNe 2005hk, 2008ha and SN 2010ae (Stritzinger et al. 2014, A&A, 561, 146), SN 2014ck (Tomasella et al. 2016, MNRAS, 459, 1018), as well as an expanded sample of SNe IaX (Foley et al. 2013, ApJ, 767, 57)., and most recently, a detailed study of their host-galaxy properties (Lyman et al. 2017, MNRAS, in press).

type Ibc supernovae

Picture on the left is entitled (by eso1231 - Photo Release) "A Blue Whirlpool in The River" and was made using images of NGC 1187 obtained by the VLT (+ FORS) as a part of my late phase followup program of the type Ib supernova 2007Y.
I have worked on stripped-envelope (SE) core-collapse supernovae (SNe) from the beginning of my career. This includes the detailed studies on SN 1999ex (Stritzinger et al. 2002; including the first detection of shock break out), SN 2007Y (Stritzinger et al. 2009), SN 2009bb (Pignata, Stritzinger et al. 2010), and among others, a sample of 34 well-observed SE SNe followed by the Carnegie Supernova Project. To date a 3 of a series of 4 papers have been published based on these data (Stritzinger et al.2017a, Stritzinger et al. 2017b, Taddia et al. 2017). Currently we are using machine learning techniques to study their spectroscopic properties and to devise a more robust way to spectroscopic classify SE SNe.

Spectrophotometric Standards

In Stritzinger et al. (2005), PASP, 117, 810, we present CCD observations of 102 Landolt standard stars obtained with the Ritchey-Chrétien spectrograph on the CTIO 1.5-m telescope. Using stellar atmosphere models, we have extended the flux points to our six spectrophotometric secondary standards, in both the blue and the red, allowing us to produce flux-calibrated spectra that span a wavelength range from 3050 Å to 1.1 μm. Mean differences between UBVRI spectrophotometry computed using Bessell's standard passbands and Landolt's published photometry were determined to be 1% or less. Observers in both hemispheres will find this set of data useful for flux-calibrating spectra. In addition these data serve as a powerful tool to characterize ones natural photometric system, necessary to transform natural system photometry to another user defined photometric system (S-correction), and ultimately, enables precise SNe Ia distances. The atlas can be downloaded here: Download.

Interacting supernovae


I have also worked in collaboration with Francesco Taddia on a number of interacting Type IIn supernovae. This includes a detailed study of the long-lasting SN 2005ip and SN 2006jd (Stritzinger et al. 2012, ApJ, 756, 173), an extended sample of SNe IIn observed by the CSP-I (Taddia et al. 2013, A&A, 555, 10), as well as on the interacting Type Ia+CSM SN 2008J (Taddia et al. 2012, A&A, 545L, 7).


A couple objects of interest


The long-lasting Type IIn supernova 2006jd

The broad-line Type Ic supernova 2009bb